Download PARKER WORKSHOP ON MAGNETIC RECONNNECTION

PARKER WORKSHOP ON MAGNETIC RECONNNECTION Workshop in honor of Eugene N. Parker to be held at the National Institute of Space Research, INPE, São José dos Campos, SP, Brazil, during March 18-21, 2014. PROGRAM & ABSTRACTS Edited by: Walter D. Gonzalez Alarcon Alicia L. Clúa de Gonzalez Daiki Koga Marcos Vinicius Dias Silveira Arian Ojeda González INPE, São José dos Campos, SP, Brazil March 2014 Organizer: Sponsors: 2 Scientific Organizing Committee Eugene Parker (University of Chicago, USA) Masaaki Yamada (Princeton Plasma Physics Laboratory, USA) Eric Priest (St. Andrews University, UK) Forrest Mozer (University of California, Berkeley, USA) Vytenis Vasyliunas (Max Planck Institute, Germany) Jim Drake (University of Maryland, USA) Michael Hesse (Goddard Space Flight Center, USA) Paul Cassak (West Virginia University, USA) Homa Karimabadi (University of California, San Diego, USA) Amitava Battacharjee (University of New Hampshire, USA) Alex Lazarian (University of Wisconsin, Madison, USA) William Daughton (Los Alamos National Laboratory, USA) Gunnar Horning (University of Dundee, UK) Michael Shay (University of Delaware, USA) Kazunari Shibata (University of Kyoto, Japan) Ray Walker (University of California, LA, USA) Merav Opher (Boston University, USA) Philip Pritchett (University of California, LA, USA) Dimitri Usdenky (University of Colorado, USA) Jack Scudder (University of Iowa, USA) Walter D. Gonzalez Alarcon (INPE, SP, Brazil) Local Organizing Committee Walter D. Gonzalez Alarcon (INPE, SP, Brazil) Alicia L. Clúa de Gonzalez (INPE, SP, Brazil) José Humberto A. Sobral (INPE, SP, Brazil) Alisson Dal Lago (INPE, SP, Brazil) Maria Virginia Alves (INPE, SP, Brazil) Odim Mendes (INPE, SP, Brazil) Daiki Koga (INPE, SP, Brazil) Arian Ojeda González (INPE and bolsista do CNPq, SP, Brazil) Mariza P. de Souza Echer (INPE, SP, Brazil) Flávia Reis Cardoso (INPE and Univ. de Lorena, SP, Brazil) Marcos Vinicius Dias Silveira (INPE, SP, Brazil) Cristiane Loesch de Souza Costa (INPE, SP, Brazil) Germán Fariñas Pérez (INPE, SP, Brazil) Fabiola Pinho Magalhães (INPE, SP, Brazil) CONTENTS Pág. 1 SCIENTIFIC PROGRAM . . . . . . . . . . . . . . . . . . . . . . . 2 2 TUTORIAL PRESENTATIONS . . . . . . . . . . . . . . . . . . . 7 3 POSTER CONTRIBUTIONS . . . . . . . . . . . . . . . . . . . . . 12 4 ABSTRACTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17 4.1 Tutorial Presentation Abstracts . . . . . . . . . . . . . . . . . . . . . . . 17 4.2 Poster Contribution Abstracts . . . . . . . . . . . . . . . . . . . . . . . . 64 5 DISCUSSION . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 106 6 LIST OF PARTICIPANTS . . . . . . . . . . . . . . . . . . . . . . 112 1 1 SCIENTIFIC PROGRAM DAY-1, Tuesday, 18 March, 2014 08 : 30 − 09 : 00 “Registration” 09 : 00 − 09 : 30 “Opening Ceremony” - Dr. Leonel Fernando Perondi, Director of INPE 09 : 30 − 10 : 00 “Opening Talk” (E. N. Parker) 10 : 00 − 10 : 20 Coffee Break 10 : 20 − 12 : 25 SESSION 1 (Fundamental Concepts), Chair: V. Vasyliunas 10 : 20 − 10 : 45 “Empirical Constructs Associated With Magnetic Field Reconnection”, Forrest S. Mozer 10 : 45 − 11 : 10 “On the General Nature of 3D Reconnection”, E. R. Priest 11 : 10 − 11 : 35 “Analytical approach in time-dependent magnetic reconnection of skewed magnetic fields”, V. S. Semenov 11 : 35 − 12 : 00 “Collisionless reconnection in the solar corona”, Jörg Büchner 12 : 00 − 12 : 25 “Indeterminacy and instability in Petschek reconnection”, Terry Forbes 12 : 25 − 14 : 00 Lunch 14 : 00 − 16 : 05 SESSION 2 (Coronal Heating, Energetics, Plasmoids and Jets), Chair: E. Priest 14 : 00 − 14 : 25 “Current sheets formation and the heating of solar and stellar Coronae”, Antonio F. Rappazzo 14 : 25 − 14 : 50 “Turbulent relaxation of braided magnetic fields”, Gunnar Hornig 14 : 50 − 15 : 15 “Plasmoid-Induced-Reconnection and Fractal Reconnection in Solar-Flare”, Kazunari Shibata 15 : 15 − 15 : 40 “Fast Reconnection Mediated by the Plasmoid Instability in HighLundquist-Number Plasmas: Dynamics and Statistics”, Amitava Bhattacharjee 15 : 40 − 16 : 05 “The structure of the diffusion region in collisionless reconnection: Theory, simulation, and observation”, Seiji Zenitani 16 : 05 − 16 : 30 Coffee Break 16 : 30 − 18 : 10 SESSION 2 (Continuation...), Chair: E. Priest 16 : 30 − 16 : 55 “Recent observations of solar flares“, Hugh Hudson 16 : 55 − 17 : 20 “Analysis of solar flares from microwaves to THz frequencies and challenges for interpretation”, Pierre Kaufmann 2 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 17 : 20 − 17 : 45 “Analysis of the reconnection processes responsible for the 3D jet phenomena in the solar coronal holes”, Klaus Galsgaard 17 : 45 − 18 : 10 “Effects of electron inertia in Hall-MHD magnetic reconnection”, Daniel Gomez DAY-2, Wednesday, 19 March, 2014 09 : 00 − 19 : 00 Information Workshop Trip On wednesday 19 (local holiday) there will be a tour for the participants of the Workshop to a near beach (Ubatuba). The tour will depart Ibis hotel at 08:30 hr and return by 19:00 hr. At the beach there will be an optional ship cruse around some islands near Ubatuba, with a duration of about two hours. The lunch at Ubatuba will be at the hotel Ancoradouro (http://www.pousadaancoradouro.com.br/localizacao.htm), with several choices at the menu. The recreation areas at the hotel, including the swimming pool, will be available for the Workshop participants. Please, notice that the beach is also suitable for swimming. Map: Instituto Nacional de Pesquisas Espaciais - INPE 3 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil DAY-3,Thursday, 20 March, 2014 08 : 30 − 10 : 10 SESSION 3 (Diffusion Region and Particle Acceleration), Chair: M. Yamada 08 : 30 − 08 : 55 “Study of Particle Energization during Magnetic Reconnection in a Laboratory Plasma”, Masaaki Yamada 08 : 55 − 09 : 20 “The Diagnostic Role of Electrons in Collisionless Reconnection”, Jack D. Scudder 09 : 20 − 09 : 45 “Observation of electron acceleration in the separatrix region during magnetic reconnection”, Rongsheng Wang 09 : 45 − 10 : 10 “Multi-Scale Simulations of Electron Energization in Earth’s Magnetotail”, Maha AshourAbdalla 10 : 10 − 10 : 30 Coffee Break 10 : 30 − 12 : 35 SESSION 4 (Turbulence), Chair: William Daughton 10 : 30 − 10 : 55 “Emerging Connections between Turbulence and Magnetic Reconnection in Collisionless Plasmas”, William Daughton 10 : 55 − 11 : 20 “Spontaneous Stochasticity & Turbulent Magnetic Reconnection”, Gregory L. Eyink 11 : 20 − 11 : 45 “Turbulent Reconnection”, Alex Lazarian 11 : 45 − 12 : 10 “Fast Magnetic Reconnection in Turbulent Media”, Grzegorz Kowal 12 : 10 − 12 : 35 “The role of Magnetic Reconnection on Cosmic Ray Acceleration”, Elizabete de Gouveia Dal Pino 12 : 35 − 14 : 00 Lunch 14 : 00 − 16 : 05 SESSION 5 (Solar Wind-Magnetosphere Coupling), Chair: Forrest S. Mozer 14 : 00 − 14 : 25 “The Axford Conjecture and the Properties of an Open Magnetosphere”, Vytenis W. R. Vasyliunas 14 : 25 − 14 : 50 “Quantitative Predictions of Magnetic Reconnection at the Dayside Magnetopause”, Paul Cassak 14 : 50 − 15 : 15 “The Role of Magnetic Reconnection at the Dayside Magnetopause: From one of Many Processes to the Dominant one”, Stephen A. Fuselier 15 : 15 − 15 : 40 “Assessing the Validity of the Maximum Magnetic Shear Model: A Review“, Karlheinz Trattner Instituto Nacional de Pesquisas Espaciais - INPE 4 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 15 : 40 − 16 : 05 “Role of reconnection in energy input from solar wind to the magnetosphere - ionosphere system”, Tuija Pulkkinen 16 : 05 − 16 : 30 Coffee Break 16 : 30 − 17 : 20 SESSION 5 (Continuation...), Chair: Forrest S. Mozer 16 : 30 − 16 : 55 “Generation of the ionospheric transpolar potential”, Ramón Lopez 16 : 55 − 17 : 20 “Fluid and Kinetic signatures of reconnection at the dayside magnetopause observed by Double Star TC1”, Lorenzo Trenchi 17 : 20 − 17 : 50 Poster Session 19 : 30− Workshop Dinner DAY-4, Friday, 21 March, 2014 08 : 30 − 10 : 10 SESSION 6 (Magnetotail Onset, Transients Ionosphere and Aurora), Chair: Gerhard Haerendel 08 : 30 − 08 : 55 “The Onset of Magnetic Reconnection in the Presence of a Finite Normal Magnetic Field Component”, Philip Pritchett 08 : 55 − 09 : 20 “Double Layers and Strong Guide Field Magnetic Reconnection in low Beta Plasmas”, Robert Ergun 09 : 20 − 09 : 45 “Reconnection signatures in the Earth’s magnetotail observed by multi-point spacecraft”, Rumi Nakamura 09 : 45 − 10 : 10 ‘Magnetotail current sheet: multiscale equilibrium structure and stability”, Anatoli Petrukovich 10 : 10 − 10 : 30 Coffee Break 10 : 30 − 12 : 10 SESSION 6 (Continuation...), Chair: Gerhard Haerendel 10 : 30 − 10 : 55 “Kinetic Simulations and Theory of Wave Generation and Particle Acceleration at Reconnection-Generated Dipolarization Fronts”, Richard D. Sydora 10 : 55 − 11 : 20 “Size and shape of the distant magnetotail”, David Sibeck 11 : 20 − 11 : 45 “A Revolutionary Aeronomy Concept to Explore the Coupling of the Solar-Terrestrial System”, James F. Spann 11 : 45 − 12 : 10 “Field line resonance trigger auroral arcs identified by ground and multi-spacecraft in the near-Earth mangetotail”, A.M. Du 12 : 10 − 14 : 00 Lunch Instituto Nacional de Pesquisas Espaciais - INPE 5 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 14 : 00 − 16 : 05 SESSION 7 (Other Reconnection Scenarios), Chair: K. Shibata 14 : 00 − 14 : 25 “Magnetic Fractures or Reconnection of Type II”, Gerhard Haerendel 14 : 25 − 14 : 50 “Simulation Studies of Plasma Transport at the Earth and Outer Planets”, Ray Walker 14 : 50 − 15 : 15 “Moving Beyond Standard Global Descriptions of the Heliosphere: Reconnection in the Heliosheath and Heliopause”, Merav Opher 15 : 15 − 15 : 40 “Radiative Magnetic Reconnection in Astrophysics”, Dmitri A. Uzdensky 15 : 40 − 16 : 05 “Annihilation of Quantum Magnetic Fluxes in Superconducting Systems and Neutron Stars”, W. D. Gonzalez 16 : 05 − 16 : 30 Coffee Break 16 : 30 − 17 : 30 DISCUSSION (See questions in Chapter 5) CLOSING 17 : 30 Instituto Nacional de Pesquisas Espaciais - INPE 6 2 TUTORIAL PRESENTATIONS Ref. Titles and authors Pg. T1 Multi-Scale Simulations of Electron Energization in Earth’s 18 Magnetotail - Maha Ashour-Abdalla, Giovanni Lapenta, Mostafa ElAlaoui and Raymond J. Walker T2 Fast Reconnection Mediated by the Plasmoid Instability in 20 High-Lundquist-Number Plasmas: Dynamics and Statistics Amitava Bhattacharjee, L. Guo, Y.-M. Huang, and Davina Innes T3 Collisionless Reconnection in the Solar Corona - Jörg Büchner T4 Quantitative Predictions of Magnetic Reconnection at the Day- 22 side Magnetopause - Paul A. Cassak T5 Emerging Connections between Turbulence and Magnetic Re- 23 connection in Collisionless Plasmas - William Daughton T6 Field Line Resonance Trigger Auroral Arcs Identified by 24 Ground and Multi-Spacecraft in the Near-Earth Magnetotail - Ai-Min Du, and T.L. Zhang T7 Double Layers and Strong Guide Field Magnetic Reconnection in low Beta Plasmas - Robert Ergun 25 T8 Spontaneous Stochasticity & Turbulent Magnetic Reconnection - Gregory L. Eyink 26 T9 Intermittency and Instability in Petschek Reconnection - 27 Terry G. Forbes 7 21 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T10 The Role of Magnetic Reconnection at the Dayside Magne- 28 topause: From one of Many Processes to the Dominant one Stephen A. Fuselier T11 Analysis of the Reconnection Processes Responsible for the 3D 29 Jet Phenomena in the Solar Coronal Holes - Klaus Galsgaard T12 Effects of Electron Inertia in Hall-MHD Magnetic Reconnection 30 - Daniel O. Gomez T13 Magnetic Fractures Gerhard Haerendel T14 Turbulent Relaxation Gunnar Hornig T15 Recent Observations of Solar Flares - Hugh Hudson 33 T16 Turbulent Reconnection - Alexandre Lazarian 34 T17 Generation of Ramon E. Lopez T18 Empirical Constructs Associated With Magnetic Field Recon- 36 nection - Forrest S. Mozer T19 Reconnection Signatures in the Earth’s Magnetotail Observed 37 by Multi-point Spacecraft - Rumi Nakamura T20 Moving Beyond Standard Global Descriptions of the Helio- 38 sphere: Reconnection in the Heliosheath and Heliopause Merav Opher T21 Magnetic Field Line Topology and Magnetic Reconnection - 39 Eugene N. Parker the or of Reconnection Braided Ionospheric of Type Magnetic Transpolar II - 31 Fields - 32 Potential Instituto Nacional de Pesquisas Espaciais - INPE - 35 8 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T22 Magnetotail Current Sheet: Multiscale Equilibrium Structure 40 and Stability - Anatoli A. Petrukovich, L.M. Zelenyi, A.V. Artemyev, H.V. Malova T23 On the General Nature of 3D Reconnection - Eric R. Priest T24 The Onset of Magnetic Reconnection in the Presence of a Finite 42 Normal Magnetic Field Component - Philip L. Pritchett T25 Role of Reconnection in Energy Input from Solar Wind to the Magnetosphere-Ionosphere System - Tuija I. Pulkkinen T26 Current Sheets Formation and the Heating of Solar and Stellar 44 Coronae - Franco Rappazzo T27 In Situ Observations of Magnetic Reconnection in Solar System 45 Plasmas - Alessandro Retinò, A. Chasapis, C. Rossi, F. Sahraoui, L. Hadid, A. Vaivads, Y. Khotyaintsev, R. Nakamura , B. Zieger, D. Sundkvist, F. S. Mozer, M. Fujimoto, S. Kasahara, A. Masters, H. Fu T28 The Diagnostic Role of Electrons in Collisionless Reconnection 46 - Jack D. Scudder T29 Analytical Approach in Time-dependent Magnetic Reconnec- 47 tion of Skewed Magnetic Fields - V. S. Semenov T30 Plasmoid-Induced-Reconnection and Fractal Reconnection in 48 Solar Flares - Kazunari Shibata T31 Size and Shape of the Distant Magnetotail - David G. Sibeck T32 A Revolutionary Aeronomy Concept to Explore the Coupling 50 of the Solar-Terrestrial System - James F. Spann Instituto Nacional de Pesquisas Espaciais - INPE 41 43 49 9 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T33 Kinetic Simulations and Theory of Wave Generation and Par- 51 ticle Acceleration at Reconnection-Generated Dipolarization Fronts - Richard D. Sydora, Maha Ashour-Abdalla, Meng Zhou, and Raymond J Walker T34 Assessing the Validity of the Maximum Magnetic Shear Model: 52 A Review - Karlheinz J. Trattner T35 Fluid and Kinetic Signatures of Reconnection at the Dayside 53 Magnetopause Observed by Double Star TC1 - Lorenzo Trenchi T36 Radiative Magnetic Dmitri Uzdensky T37 The Axford Conjecture and the Properties of an Open Magne- 55 tosphere - Vytenis M. Vasyliunas T38 Simulation Studies of Plasma Transport at the Earth and Outer 56 Planets - Raymond J. Walker, Keiichiro Fukazawa, and Tatsuki Ogino T39 Parallel Electric Fields and Subcavities in Magnetotail Recon- 57 nection (assumed title) - Rongsheng Wang T40 Study of Particle Energization during Magnetic Reconnection in a Laboratory Plasma - Masaaki Yamada T41 The Structure of the Diffusion Region in Collisionless Recon- 59 nection: Theory, Simulation, and Observation - Seiji Zenitani T42 The Role of Magnetic Reconnection on Cosmic Ray Accelera- 60 tion - Elizabete de Gouveia Dal Pino T43 Analysis of Solar Flares from Microwaves to THz Frequencies 61 and Challenges for Interpretation - Pierre Kauffmann Reconnection in Astrophysics Instituto Nacional de Pesquisas Espaciais - INPE - 54 10 58 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T44 Fast Magnetic Grzegorz Kowal Reconnection in Turbulent Media T45 Annihilation Of Quantum Magnetic Fluxes in Superconducting 63 Systems and Neutron Stars - Walter D. Gonzalez Instituto Nacional de Pesquisas Espaciais - INPE - 62 11 3 POSTER CONTRIBUTIONS Ref. Titles and authors Pg. P1 Energetic Protons Cross-Field Diffusion in the Heliosphere - 65 Edio da Costa Junior, Bruce T. Tsurutani, Maria Virgı́nia Alves, Ezequiel Echer and Gurbax S. Lakhina P2 Solar Mean Flows and Dynamo, a Critical, Updated, Review - 66 Gustavo Guerrero P3 Solar Flares Observed with POEMAS - Adriana Válio, P. Kauf- 67 mann, C. Guillermo Giménez de Castro P4 Statistical Analysis of Radar Observed F Region Irregularities 68 from Three Longitudinal Sectors - R. Y. C. Cueva, E. R. de Paula, and A. E. Kherani P5 Magnetopause Reconnection and Interlinked Flux Tubes - 69 F. R. Cardoso, W. D. Gonzalez, D. G. Sibeck, M. Kuznetsova, and D. Koga P6 Transport Barriers In Confined Plasmas - Iberê Luiz Caldas P7 The Role of Magnetic Activity and Reconnection on the 17 Radio and Gamma-Ray Emission of Compact Sources Luı́s H.S. Kadowaki and Elisabete M. de Gouveia Dal Pino P8 A Magnetic Reconnection Model for Explaining AGNs and Mi- 72 croquasars Radiation - B. Khiali, E.M. de Gouveia Dal Pino, M. V. del Valle, G. Kowal , H. Sol 12 70 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P9 Spectrum of Electromagnetic Waves Obtained as Asymptotic 73 Quasi-equilibrium Solution of the Equations of the Theory of Weak Turbulence in Unmagnetized Plasmas - L. F. Ziebell, Peter H. Yoon, R. Gaelzer, J. Pavan, and F. J. R. Simões Jr. P10 Temperature-Anisotropy-Driven Instabilities Generated by the 75 Superthermal Distributions Observed in the Solar Wind R. Gaelzer, L. F. Ziebell, and M. S. dos Santos P11 PIC Simulations of Electrostatic Harmonic Emissions in Space 77 Plasmas - F. C. H. Machado, F. J. R. Simões Jr., M. V. Alves P12 Universal Scaling Laws for Fully-Developed Magnetic Field Tur- 78 bulence Near and Far Upstream of the Earth’s Bow Shock Rodrigo A. Miranda, Abraham C.-L. Chian, Erico L. Rempel P13 A Plasma Thruster Based on Aurora Type Particle Accelera- 79 tion Mechanisms - José Leonardo Ferreira, Artur Castelo Branco Santos Serra and Aderson Lucas Medeiros P14 Escape Pattern and Stickiness in a Poloidally Diverted Tokamak 81 - Caroline G. L. Martins, M. Roberto and I. L. Caldas P15 Detection of Coherent Structures in Space Plasmas and its Re- 82 lation with Solar Wind Turbulence and Magnetic Reconnection - Pablo R. Muñoz and A. Ojeda González P16 Interplanetary Origin of Geomagnetic Storms (Peak Dst −50nT ) 83 During the Solar Cycle 23 - E. Echer, W. D. Gonzalez, and B. T. Tsurutani P17 A Double-Cored FTE from BATS-R-US - Aline de Lucas, D. 84 Sibeck, W.D. Gonzalez, and M.V. Silveira Instituto Nacional de Pesquisas Espaciais - INPE 13 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P18 HILDCAAs and Associated Interplanetary Variations: Super- 85 posed Epoch Analyses Under Varying Solar Activity and Seasonal Conditions - Rajkumar Hajra, Ezequiel Echer, Walter D. Gonzalez, and Bruce T. Tsurutani P19 Extended Dayside Magnetopause Reconnection Line as Ev- 86 idenced by Quasi-Simultaneous THEMIS Observations Vitor Souza, Walter Gonzalez, David Sibeck, Brian Walsh, Daiki Koga and Odim Mendes P20 A Review on Coronal Heating Problem - S. S. A. Silva, M. V. Alves and J. C. Santos P21 The Io Plasma Torus - Fabiola Pinho Magalhães, Walter D. Gonzalez, 88 Mariza P. S. Echer, and Ezequiel Echer P22 Global Muon Detector Network - Cosmic Rays as Other Point 89 of View for Space Weather’s Applications - Rockenbach, M., Dal Lago, A., Schuch, N.J., Munakata, K., Kuwabara, T., Oliveira, A.G., E. Echer, Braga, C.R., Mendonça, R.R.S., Kato C., Yasue, S., Tokumaru, M., Bieber, J.W., Evenson P., Duldig, M. L., Humble, J. E., Al Jassar, H. K., Sharma M. M., Sabbah, I. P23 A Comparative Study of Lagrangian Techniques for De- 91 tecting Coherent Structures in the Solar Photosphere Jenny M. Rodrı́guez, Abraham C.-L. Chian and Erico L. Rempel P24 Comparative Study of the Magnetic and Plasma Pressure 92 Forces in the Magnetosheath - Germán Fariñas Pérez, Walter D. Gonzalez, Flavia R. Cardoso, and Ramon E. Lopez P25 Validation of the Reconnection Component Model and Deter- 93 mination of the Reconnection X- Line for Different Configurations of the Interplanetary Magnetic Field Using the 3D MHD BATS-R-US Model - Paulo Ricardo Jauer, Walter D. Gonzalez, and Cristiane Loeschen Instituto Nacional de Pesquisas Espaciais - INPE 14 87 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P26 Hall Electric Field in Asymmetric Magnetic Reconnection - 94 D. Koga, W. D. Gonzalez, F. S. Mozer, and F. R. Cardoso P27 Observation of Fundamental Magnetopause Reconnection Pa- 95 rameters by the POLAR Satellite - Walter D. Gonzalez, Daiki Koga, Barbara Ribeiro, Forrest Mozer, Paul Cassak, and Jack Scudder P28 Magnetic Field and Flow Variations Associated with a Tran- 96 sient Event Observed at the Magnetopause by the THEMIS Spacecraft - M. V. D. Silveira, D. G. Sibeck, W. D. Gonzalez, and D. Koga P29 Characterization of a Double Flux-Rope Magnetic Cloud 97 Observed by ACE Spacecraft on August 19-21, 1998 A. Ojeda González, W. D. Gonzalez, O. Mendes, M. O. Domingues, and P. R. Muñoz P30 3D Hall Mhd Global Simulation of the Magnetopause Response 98 to the April, 2010 Event: Analysis of Possible Magnetic Reconnection Regions - C. Loesch, M. V. Alves, P. R. Jauer, and W. D. Gonzalez P31 Multi-Wavelength Observation and Analysis of a Coherent, 99 Wave-Like Propagating Intensity Disturbances Along PseudoOpen Field Lines Above a Sunspot - Tardelli Stekel, Guillermo Stenborg, and Alisson Dal Lago P32 Magnetic Configuration of a Flaring Active L. Balmaceda, J. Palacios, L. E. Vieira, and A. Dal Lago P33 The Geomagnetic Response to Extreme Solar Wind Events - 101 A. Dal Lago, E. Echer, L. A. Balmaceda, R. Rawat, L. E. A. Vieira, T. R. C. Stekel and W. D. Gonzalez Region - 100 Instituto Nacional de Pesquisas Espaciais - INPE 15 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P34 Modeling the Equatorial and Low Latitude Ionosphere Re- 102 sponse to an Intense X-Class Solar Flare - P. A. B. Nogueira, J. R. Souza, M. A. Abdu, R. Paes, J. Sousasantos, M.S. Marques, R.Y.C. Cueva, C.M. Denardini, I.S. Batista, H. Takahashi, and S.S. Chen P35 Storm Electric Field effects in the low-latitude Ionosphere - 103 J. R. Souza, B. G. Fejer, M. A. Abdu, I. S. Batista, and G. J. Bailey P36 Simulation of Ideal MHD Model in the Context of Adap- 104 tive Multiresolution Using the Hyperbolic Divergence Cleaning Approach - Anna Karina F. Gomes, Margarete O. Domingues, Odim Mendes, Kai Schneider P37 Degradation of the Magnetic Structure of Elongated ICMEs by 105 Interior Reconnection - Raymond L. Fermo, M. Opher, J. F. Drake Instituto Nacional de Pesquisas Espaciais - INPE 16 4 ABSTRACTS 4.1 Tutorial Presentation Abstracts 17 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T1) MULTI-SCALE SIMULATIONS OF ELECTRON ENERGIZATION IN EARTH’S MAGNETOTAIL Maha Ashour-Abdalla[1] , Giovanni Lapenta, Mostafa El-Alaoui and Raymond J. Walker [1] IGPP, University of California, Los Angeles, USA. e-mail: [email protected] ABSTRACT Using data from the THEMIS and Cluster missions together with global and test particle simulations, we demonstrate that electrons are accelerated in two distinct regions. In a study of a substorm on February 15, 2008 we used the large scale kinetic simulation approach in which particle trajectories are followed in the electric and magnetic fields from a global magnetohydrodynamic simulation to show that a low energy population (up to a few keV) appears to arise in the diffusion region where particles are demagnetized and the magnetic topology changes. In addition a high energy component that is energized by adiabatic processes (mostly betatron acceleration) arises within dipolarization fronts as they sweep toward the inner magnetosphere far from the diffusion region. This study concluded that particle energization during substorms is not associated solely with the conversion of magnetic to kinetic energy but, also arises in conjunction with macroscopic flows. In a substorm, on March 11, 2008 we extended this work and found that the LSK results compared favorably with observations only when we added a high energy tail to the distribution function near the reconnection site. This implies that acceleration near the X-line was substantial and needs to be included. In addition THEMIS and Cluster observations indicate that plasma waves are associated with the dipolarization fronts. The LSK approach is not self-consistent and does not include plasma waves. Therefore, to fully understand the processes that lead to electron acceleration throughout the near-Earth tail, we need to utilize a self-consistent kinetic approach that includes waves and electron acceleration near the neutral line along with the large-scale dynamics. In this talk we present results from a model which couples the large scale magnetospheric processes and kinetic processes by developing a simulation approach in which a global MHD simulation is coupled with a particle in cell simulation. In this approach we couple the UCLA global MHD code with an implicit particle in cell code called iPIC3D. In the first case study we use a two dimensional version of iPIC3D to investigate the multi-scale nature of the electron energization during the February 15, 2008 substorm. In this multi-scale simulation the electric and magnetic fields show a quadrupole signature of Hall-MHD, absent Instituto Nacional de Pesquisas Espaciais - INPE 18 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil in the resistive MHD case. Moreover the electrons move much faster than the ions especially at the separatrices and the inflow boundary. We note that during this event, just like in the case of the MHD, dipolarization fronts are formed mainly earthward of the neutral line. Finally, we find that electrons are energized near both the x-line and dipolarization fronts, but the energization is greater at the latter location. Instituto Nacional de Pesquisas Espaciais - INPE 19 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T2) FAST RECONNECTION MEDIATED BY THE PLASMOID INSTABILITY IN HIGH-LUNDQUIST-NUMBER PLASMAS: DYNAMICS AND STATISTICS Amitava Bhattacharjee[1] , L. Guo, Y.-M. Huang, and Davina Innes [1] Princeton University, USA. e-mail: [email protected] ABSTRACT In this talk, we will review some recent developments in the theory and simulation of the plasmoid instability, which addresses foundational issues in nonlinear reconnection theory, to which Professor Eugene Parker has made seminal contributions. These developments stem from the realization that underlying the canonical Sweet-Parker model, there is an underlying assumption that the system-size current sheet mediating reconnection in resistive plasmas is stable. Recent work has shown that above a critical threshold in Lundquist number, the SweetParker current sheet is violently unstable to a secondary, super-Alfvenic tearing instability (called the plasmoid instability) that produces, rather remarkably, a nonlinear regime in which the reconnection rate becomes independent of the Lundquist number. Inclusion of Hall MHD effects changes qualitatively the nonlinear regimes accessible to the plasma. One of the regimes is X-point like, but when the system size becomes sufficiently large, there is a novel regime in which the current sheet geometry alternates dynamically between two meta-stable states: an X-point and an extended thin current sheet unstable to the plasmoid instability. Recently, we have developed a theoretical model for the statistical distribution of plasmoids in quasi-steady state. A new kinetic equation has been developed for the plasmoid distribution function f (Ψ) (where Ψ is the flux trapped in a plasmoid), which predicts a power-law f (Ψ) ∼ Ψ − 1, consistent with simulation results. These results have been tested recently with coronal observations of post-CME heliospheric current sheets and supra-arcade downflows. Instituto Nacional de Pesquisas Espaciais - INPE 20 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T3) COLLISIONLESS RECONNECTION IN THE SOLAR CORONA Jörg Büchner[1] [1] Max Planck Institute, Germany. e-mail: [email protected] ABSTRACT Solar eruptions and even the heating of the corona is widely believed to be due to the release of magnetic energy in this essentially low-beta plasma. Since the Spitzer resistivity in the solar corona is small the corresponding magnetic Reynolds numbers are large. Hence the energy release by magnetic reconnection has to be an essentially collisionless process. We discuss how collisionless reconnection might yield energy conversion rates as fast as 0.1 Va B, where B is the upstream magnetic field and Va the corresponding Alfvén velocity. Instituto Nacional de Pesquisas Espaciais - INPE 21 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T4) QUANTITATIVE PREDICTIONS OF MAGNETIC RECONNECTION AT THE DAYSIDE MAGNETOPAUSE Paul A. Cassak[1] [1] West Virginia University, USA. e-mail: [email protected] ABSTRACT Despite over 50 years of research, surprisingly little can be quantitatively predicted about magnetic reconnection at the dayside magnetopause for arbitrary conditions in the solar wind. Basic fundamental issues such as what controls the efficiency of dayside reconnection and where dayside reconnection even occurs have not been answered satisfactorily. One of the many complications making this problem particularly difficult is the apparent dependence on both local and global considerations. This talk will describe recent theoretical and numerical efforts to understand dayside reconnection using both local and global approaches. At the local scale, dayside reconnection is known to have asymmetric magnetic fields and densities, as well as shear flows depending on where it is located. Efforts to predict how these effects impact traditional models of reconnection will be discussed. At the global scale, recent efforts to locate magnetic reconnection sites in global magnetohydrodynamic magnetospheric simulations will be discussed, including a careful systematic test of a number of leading models of the location of dayside reconnection for multiple sets of conditions in the solar wind. As understanding dayside reconnection is important for predicting the coupling of the solar wind to the magnetosphere and driving space weather phenomena, this line of research is very important. Observational implications will be discussed. Instituto Nacional de Pesquisas Espaciais - INPE 22 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T5) EMERGING CONNECTIONS BETWEEN TURBULENCE AND MAGNETIC RECONNECTION IN COLLISIONLESS PLASMAS William Daughton[1] [1] Los Alamos National Laboratory, USA. e-mail: [email protected] ABSTRACT Magnetic reconnection is a fundamental process that often results in an explosive release of energy as magnetic fields are reconfigured and destroyed in high temperature plasmas. This process plays a central role in diverse applications such as solar flares, planetary magnetospheres, laboratory experiments and a growing number of astrophysical problems. Many of the scientific challenges in understanding reconnection are related to the vast separation between the macroscopic scales of interest and the underlying kinetic scales, where the frozen-flux condition is violated in hot plasmas. As a result, most kinetic studies have been limited to two-dimensional models for laminar conditions. This is beginning to change with the advent of petascale computers, which have enabled a factor of 1000 increase in the size of kinetic simulations over the past 5 years. These advancements are leading to some major breakthroughs in our understanding of magnetic reconnection and the spontaneous generation of turbulence. This talk will present an overview of these new results with an emphasis on parameter regimes relevant to the Earth’s magnetosphere. Evidence for these new predictions from spacecraft data will be discussed along with opportunities for detailed validation comparisons with upcoming NASA missions and laboratory experiments. Instituto Nacional de Pesquisas Espaciais - INPE 23 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T6) FIELD LINE RESONANCE TRIGGER AURORAL ARCS IDENTIFIED BY GROUND AND MULTI-SPACECRAFT IN THE NEAREARTH MAGNETOTAIL Ai-Min Du[1] , and T.L. Zhang [1] Geophysical Institute, Chinese Academy of Sciences, Beijing, China. e-mail: [email protected] ABSTRACT Data from satellite THEMIS, GOES11 and ground-based magnetometers are used to investigate characteristics of field line resonance (FLR) in ionosphere and the plasma sheet. The Pi2 ULF waves observed by CARISMA array show the signatures of field line resonance during 0400 ∼ 0500 UT on March 9, 2009. The FLR occurred narrowly in latitude band and wide in longitude. A large amplitude Pi2 was observed by the THEMIS-A (P5) and GOES11 satellites near equator in the near-Earth magnetotail on March 9, 2008. P5 was located in X ∼ −5 Re. Firstly P5 detected a compressional wave, then a shear Alfven wave. The Alfven wave accelerated the electron to precipitate into the footprint of P5, resulted in the discrete auroral arcs. Instituto Nacional de Pesquisas Espaciais - INPE 24 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T7) DOUBLE LAYERS AND STRONG GUIDE FIELD MAGNETIC RECONNECTION IN LOW BETA PLASMAS Robert Ergun[1] [1] LASP, University of Colorado, Boulder, CO, USA. e-mail: [email protected] ABSTRACT The double layer can be viewed as a close cousin to strong guide-field magnetic reconnection, particularly in low beta plasmas. Both processes break the concept of a “magnetic field line” through a perpendicular gradient in the parallel electric field. Both processes also allow for the release of electromagnetic energy into particle acceleration and/or heating. This paper discusses the subtle differences between the double layer and strong guide magnetic reconnection and how the magnetic helicity is changed. Data from the THEMIS satellite are used to demonstrate how the two processes can be interlinked. In the central plasma sheet, double layers are observed during bursty bulk flow events, in the current sheet, and plasma sheet boundary layer, all during periods of strong magnetic fluctuations and believed to be associated with magnetic reconnection events. I discuss the possibility that parallel electric fields may be important in de-tangling magnetic field lines after reconnection. Instituto Nacional de Pesquisas Espaciais - INPE 25 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T8) SPONTANEOUS STOCHASTICITY & TURBULENT MAGNETIC RECONNECTION Gregory L. Eyink[1] [1]Johns Hopkins University, USA. e-mail: [email protected] ABSTRACT An old theme in the theory of magnetic reconnection is the uniqueness of magnetic linemotions (Newcomb, 1958). Any notion of field-line motion in ideal MHD is strictly “metaphysical” because no experiment can even in principle distinguish one motion law from another. However, line-motion laws do have observable consequences —in particular conservation of flux through co-moving loops—which open them to empirical falsification. When there are non-ideal terms in Ohm’s law for a plasma fluid, there may be no deterministic line motion whatsoever which is consistent with the evolution of the magnetic field. Nevertheless, in the limit of high-magnetic-Reynolds number turbulence one can expect that the plasma is ”near-ideal” and flux-freezing concepts will again be useful. A new difficulty emerges, however, because the ”rough” velocity fields in plasma turbulence associated to power-law spectra imply non-unique fluid particle trajectories which are as random as those in quantum mechanics! We review current evidence for such ”spontaneous stochasticity” of particle motion in fluid and MHD turbulence. Because of this effect, flux-freezing in MHD turbulence also becomes intrinsically stochastic. When the stochasticity of flux-freezing is taken into account the Lazarian-Vishniac (1999) reconnection theory becomes the natural turbulent analogue of the laminar Sweet-Parker (1958) theory. Instituto Nacional de Pesquisas Espaciais - INPE 26 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T9) INTERMITTENCY AND INSTABILITY IN PETSCHEK RECONNECTION Terry G. Forbes[1] [1] University of New Hampshire, USA. e-mail: [email protected] ABSTRACT Two puzzling aspects of Petschek’s model for fast reconnection are considered. One is its failure to occur in plasma simulations with uniform resistivity. The other is its inability to provide anything more than an upper limit for the reconnection rate. Recently, it has been discovered that previously published analytical solutions based on Petschek’s model are structurally unstable if the electrical resistivity is uniform. The structural instability is associated with the presence of an essential singularity at the X-line that is unphysical. By requiring that such a singularity not exist, we obtain a formula that predicts a specific rate of reconnection. For uniform resistivity, reconnection can only occur at the slow, Sweet-Parker rate. For nonuniform resistivity reconnection can occur at much faster rates in a manner that is consistent with numerical simulations. Some resistivity profiles lead to asymmetric solutions even when the profile, itself, is symmetric. These asymmetric solutions constitute examples of spontaneous symmetry breaking. Instituto Nacional de Pesquisas Espaciais - INPE 27 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T10) THE ROLE OF MAGNETIC RECONNECTION AT THE DAYSIDE MAGNETOPAUSE: FROM ONE OF MANY PROCESSES TO THE DOMINANT ONE Stephen A. Fuselier[1] [1] Southwest Research Institute, USA. e-mail: [email protected] ABSTRACT When first conceived, magnetic reconnection at the Earth’s magnetopause was considered one of several possible mechanisms for transfer of mass and energy from the magnetosheath to the magnetosphere. Other mechanisms included diffusive transfer through a variety of wave-particle interactions and “impulsive penetration” of magnetosheath plasma into the magnetosphere. As more and more evidence of reconnection was discovered, the importance of this transfer mechanism increased. Today, there is significant evidence that reconnection may never turn off at the magnetopause. The location changes with changing interplanetary magnetic field orientation, but there is strong evidence that reconnection occurs somewhere on the magnetopause all the time. Furthermore, the properties of the plasma and magnetic field in the vicinity of the magnetopause are consistent with reconnection and no other transport process is needed to explain these properties. Thus, reconnection appears to be the dominant mass and energy transfer mechanism at the magnetopause all the time. This talk presents important observational evidence that supports this claim. Instituto Nacional de Pesquisas Espaciais - INPE 28 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T11) ANALYSIS OF THE RECONNECTION PROCESSES RESPONSIBLE FOR THE 3D JET PHENOMENA IN THE SOLAR CORONAL HOLES Klaus Galsgaard[1] [1] Niels Bohr Institute, University of Copenhagen, Dennmark. e-mail: [email protected] ABSTRACT Recent spacecrafts (Hinode, Stereo and SDO) increased temporal and spacial resolution has renewed the interest in the very frequent jet phenomena taking place in coronal holes. New and more detailed numerical models have been used to provide explanations to the physical properties of these events. Magnetic reconnection is natural key component in explaining the jet properties. Fully consistent MHD experiments using the natural interaction between magnetic flux emergence into an existing coronal magnetic field have been used to investigate this process. In this talk I will review the complicated magnetic topology and its impact on the reconnection processes that takes place in the recent experiments by Moreno-Insertis & Galsgaard (Apj 771). In this experiment we find both steady state jet phase and several following explosive eruptions. Instituto Nacional de Pesquisas Espaciais - INPE 29 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T12) EFFECTS OF ELECTRON INERTIA IN HALL-MHD MAGNETIC RECONNECTION Daniel O. Gomez[1] [1] IAFE, Universidad de Buenos Aires, Argentina. e-mail: [email protected] ABSTRACT Magnetic reconnection is an important energy conversion process in highly conducting plasmas, such as those present in the solar corona or in planetary magnetospheres. Even though one-fluid magnetohydrodynamics provides the general framework for a theoretical description of reconnection, kinetic plasma effects introduce new spatial and temporal scales, which might significantly increase the reconnection rates. Within the more general framework of two-fluid MHD for a fully ionized hydrogen plasma, we retain the effects of the Hall current and electron inertia. We performed 2.5D Hall MHD simulations including electron inertia using a pseudo-spectral code which yields exact conservation (to round-off errors) of all the ideal invariants. We obtain finite reconnection rates even in the case of zero resistivity, thus showing the important influence of the electron inertia. Instituto Nacional de Pesquisas Espaciais - INPE 30 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T13) MAGNETIC FRACTURES OR RECONNECTION OF TYPE II Gerhard Haerendel[1] [1] Max Planck Institute for Extraterrestrial Physics, Garching, Germany. e-mail: [email protected] ABSTRACT The process underlying the acceleration of auroral particles at several 1000 km above the Earth is closely related to reconnection. It is based on the appearance of field-parallel voltages in the presence of intense field-aligned currents. The basic physical process is release of magnetic shear stresses, set up by the interaction of the magnetospheric with the ionospheric plasma, and conversion of the liberated magnetic energy into kinetic energy of accelerated particles. In this process field lines disconnect from the field anchored in the ionosphere and reconnect to other field lines. Because of the stiffness of the magnetic field, the process resembles mechanical fractures. Fracture propagation, or progressive erosion of magnetic shear stresses, is manifested by the proper motion of auroral arcs in the plasma frame. This process is typically active in the low density of planetary magnetospheres. It can contribute significantly to the dumping of internal or rotational energy of the magnetospheric plasma. It may also be realized in strong stellar magnetic fields and produce high-energy particles manifested as X- or gamma ray emissions. Instituto Nacional de Pesquisas Espaciais - INPE 31 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T14) TURBULENT RELAXATION OF BRAIDED MAGNETIC FIELDS Gunnar Hornig[1] [1] University of Dundee, UK. e-mail: [email protected] ABSTRACT Magnetic braiding of coronal loops due to the motion of their photospheric footpoints has long been discussed as a possible mechanism for the heating of the solar corona (E. Parker, 1972). This motivated a series of numerical experiments (Wilmot-Smith et al. 2009, 2010) on the turbulent relaxation of braided magnetic fields. These experiments have produced relaxed states which in some cases differ drastically from the predictions of the Taylor hypothesis, that is the assumption that the final state of a turbulent relaxation is a linear force-free field with the same total helicity as the initial state. We present a method to determine the topological degree of the field line mapping which shows that there are further constraints on the relaxation process beyond the conservation of the total helicity (A. Yeates et al., Phys. Rev. Lett. 105, 2010). These constraints can prevent the system from relaxing to a Taylor state and hence limit the energy which can be released. This is of interest not only for the problem of heating the solar corona but also for other relaxation processes in astrophysical plasmas. Instituto Nacional de Pesquisas Espaciais - INPE 32 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T15) RECENT OBSERVATIONS OF SOLAR FLARES Hugh Hudson[1] [1] University of California, Berkeley, USA. e-mail: [email protected] ABSTRACT Within the past few years, flare observations appear to have decisively rejected the thicktarget model for energy transport in the all-important impulsive phase of a flare. The implication of this is that the immediate consequence of magnetic energy release must have a substantial partition into ducted waves, whose Poynting flux substitutes for the hypothetical beam of the thick-target model. There are major new results on the nature of the global restructuring of the coronal field during a flare as well, and the basic problem remains roughly as Hodgson (1859) described the original white-light flare, as a ”...brilliant star of light, much brighter than the Sun’s surface”: how does the large-scale storage of energy focus into the observed small scales? Instituto Nacional de Pesquisas Espaciais - INPE 33 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T16) TURBULENT RECONNECTION Alexandre Lazarian[1] [1] University of Wisconsin, Madison, USA. e-mail: [email protected] ABSTRACT I shall discuss how magnetic reconnection is being modified in the presence of turbulence. The turbulence may pre-existing in the system and also generated by reconnection itself. I shall show how the rate of the magnetic reconnection depend on the scale on turbulence injection and the turbulent energy driving. I shall demonstrate that in magnetically dominated environments the energy release within the reconnection region leads to the ”reconnection instability” resulting in flares of reconnection provided that the initial set up has low level of turbulence. I shall discuss how the magnetic reconnection violates the magnetic flux freezing in turbulent fluids and how this changes the accepted views on the star formation and the evolution of magnetized circumstellar accretion disks. Finally, I shall discuss the acceleration of particles that the turbulent reconnection entails. Instituto Nacional de Pesquisas Espaciais - INPE 34 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T17) GENERATION OF THE IONOSPHERIC TRANSPOLAR POTENTIAL Ramon E. Lopez[1] [1] University of Texas, Arlington, USA. e-mail: [email protected] ABSTRACT As the solar wind flows past the Earth, it imposes a potential difference across the ionosphere as seen in the Earth’s frame of reference known as the transpolar potential. Two basic process, magnetic merging and a viscous interaction with the solar wind plasma, give rise to this potential. We will examine the forces on the plasmas that regulate these interactions. For the merging interaction, we shall see that the forces on the magnetosheath flow determine the amount of solar wind magnetic flux that actually reaches the merging line, and that this explains both the linear dependence of the transpolar potential on the southward component of the IMF as well as the phenomenon of transpolar potential saturation during large IMF values. For the viscous interaction, we will see how forces on the low-latitude boundary layer plasma cause the viscous interaction to weaken during periods of northward IMF. Thus, a complete understanding of how the ionospheric transpolar potential is generated must begin from the perspective of the forces acting on the plasma and the plasma flow that this produces. Instituto Nacional de Pesquisas Espaciais - INPE 35 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T18) EMPIRICAL CONSTRUCTS ASSOCIATED WITH MAGNETIC FIELD RECONNECTION Forrest S. Mozer[1] [1] Space Science Laboratory, University of California, Berkeley, USA. e-mail: [email protected] ABSTRACT An empirical construct is a model or a concept that cannot be tested by direct measurement. Examples of empirical constructs are magnetic field lines, the frozen-in condition, moving magnetic field lines and the diffusion region. While such constructs are extremely useful for visualizing physical situations, they may also be applied in domains where their solutions differ from those obtained by Maxwell’s equations and Newton’s laws of motion. This can lead to confusion and non-physical results. Examples of the use and misuse of empirical constructs will be given. Instituto Nacional de Pesquisas Espaciais - INPE 36 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T19) RECONNECTION SIGNATURES IN THE EARTH’S MAGNETOTAIL OBSERVED BY MULTI-POINT SPACECRAFT Rumi Nakamura[1] [1] Space Research Institute, Austrian Academy of Science, Austria. e-mail: [email protected] ABSTRACT Magnetic reconnection is one of the key processes in space plasmas. It converts magnetic field energy into particle energy and enables to mix plasmas from different origins. Important consequence of the magnetotail reconnection is the narrow fast plasma jets (known as bursty bulk flows), which provide the major contribution to energy and mass transport in the magnetotail. Interaction with the reconnection jets moving Earthward and the Earth’s dipole field lead to acceleration of particles, formation of the field-aligned current system, and associated auroral precipitation, and modifies the near-Earth field configuration. In this way magnetotail reconnection has also large-scale consequences as manifested during substorms. This presentation high-lights observations of the thin current sheets during magnetotail reconnection and the reconnection jet evolution obtained from multi-point measurements by Cluster and THEMIS. Depending on the spacecraft configuration, processes relevant to reconnection with different spatial/temporal scales have been observed by the spacecraft. Characteristics of the Hall-current in the ion diffusion region and a 3D nature of the localized magnetic structures in the reconnection region without guide field and with guide field are presented. A larger scale processes associated with the braking of the fast flow in the near Earth magnetosphere and formation of thin-current sheet that leads to onset of reconnection will be also discussed . Instituto Nacional de Pesquisas Espaciais - INPE 37 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T20) MOVING BEYOND STANDARD GLOBAL DESCRIPTIONS OF THE HELIOSPHERE: RECONNECTION IN THE HELIOSHEATH AND HELIOPAUSE Merav Opher[1] [1] Boston University, USA. e-mail: [email protected] ABSTRACT The sun’s solar wind carves a bubble in the interstellar medium, called the heliosphere. The recent measurements in-situ by the Voyager spacecrafts, combined with the all-sky images of the heliospheric boundaries by the Interstellar Boundary Explorer (IBEX) mission have transformed our understanding of the heliosphere. Concepts that resisted decades are being revisited due to their puzzling measurements. In particular one of the first surprises was that both Voyager found no evidence for the acceleration of the anomalous cosmic rays at the Termination Shock as expected for approximately 25 years. Another challenge are the energetically particles intensities that are dramatically different at Voyager 1 and 2. More recently, observations of Voyager 1 indicate that the spacecraft is magnetically connected to the interstellar medium while being inside the heliosheath. In this talk I will review our recent works that explore reconnection as occurring within sector region in the heliosheath and the heliopause. These works propose to explain observations that challenge the current global models to move beyond standard idealized description of the heliosphere. Our scenario of reconnection within the broad sector region explains: a) The acceleration of anomalous cosmic rays and increase in their intensity within the heliosheath until their peak intensity just before the heliopause; b) It affect the transport of particles explaining the dramatic dropouts of electrons on Voyager 2; c) Creates a flow deflection region ahead of the heliopause as seen in Voyager 1. Finally I will review on our recent suggestion that reconnection between the solar magnetic field and the interstellar magnetic field explains the dramatic dropouts and then the disappearance of the solar energetic particles. Instituto Nacional de Pesquisas Espaciais - INPE 38 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T21) MAGNETIC FIELD LINE TOPOLOGY AND MAGNETIC RECONNECTION Eugene N. Parker[1] [1] University of Chicago, USA. e-mail: [email protected] ABSTRACT Rapid reconnection of magnetic field occurs where the magnetic stresses would push the plasma and field to steepen the field gradients without bound. The physics of the thin current sheets formed in this way can be complicated, and, as detailed studies have shown, the dissipation and diffusion of magnetic field can be extremely rapid. Here we investigate the location of the rapid reconnection sites as they relate to the topology of the surrounding field. The chosen basic field form is representative of the bipolar magnetic fields in the atmosphere of the Sun, wherein the photospheric foot points are subject to ongoing mixing by the photospheric convection. We explore the simple mathematical model in which the mean field is uniform while the field lines are interlaced on small scales. We find that almost all interlacing topologies develop one or more reconnection sites. The exceptions represent a topological set of measure zero compared to all possible interlaced topologies. This simple model calculation emphasizes the universal occurrence of rapid reconnection in the re-entrant external magnetic fields of the Sun and the associated suprathermal state of the gas within. We have suggested that it is the principal cause of the X-ray corona of the S and other late main sequence stars. Instituto Nacional de Pesquisas Espaciais - INPE 39 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T22) MAGNETOTAIL CURRENT SHEET: MULTISCALE EQUILIBRIUM STRUCTURE AND STABILITY Anatoli A. Petrukovich[1] , L.M. Zelenyi, A.V. Artemyev, H.V. Malova [1] IKI, Russia. e-mail: [email protected] ABSTRACT Stability of current sheet is a critical issue for substorm initiation in the Earth’s magnetotail and one of the grand problems of space plasma physics. A new theory of anisotropic current sheets based on Cluster project observations, helped to describe quantitatively typical multilayer structure embedded within a thick plasma sheet. Such current sheet equilibrium is marginally stable (metastable) and fine details of its evolution during magnetic energy accumulation appear to be critical for the initiation of the spontaneous reconnection leading to a fast energy release. Instituto Nacional de Pesquisas Espaciais - INPE 40 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T23) ON THE GENERAL NATURE OF 3D RECONNECTION Eric R. Priest[1] [1] St Andrews University, UK. e-mail: [email protected] ABSTRACT We review the main properties of 2D and 3D reconnection, which show how different reconnection in 3D is from 2D. Also we present new results on the nature of complex topology and on the different regimes of reconnection that are possible in 3D. Instituto Nacional de Pesquisas Espaciais - INPE 41 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T24) THE ONSET OF MAGNETIC RECONNECTION IN THE PRESENCE OF A FINITE NORMAL MAGNETIC FIELD COMPONENT Philip L. Pritchett[1] [1] University of California, Los Angeles, USA. e-mail: [email protected] ABSTRACT A longstanding problem in reconnection physics is to understand how collisionless magnetic reconnection can be initiated in the presence of a finite normal Bz component, as occurs in the Earth’s magnetotail. Even a very weak Bz field magnetizes the electrons and removes the electron Landau resonance, thus ruling out the possibility of an electron tearing mode. Recent work [Sitnov and Schindler, 2010] has suggested that in an equilibrium with an accumulation of magnetic flux at the tailward end of a thin current sheet, this Bz stabilization can be reduced considerably or even eliminated. 2D and 3D particle-in-cell simulations are used to investigate the stability of such a “hump” Bz configuration. In 2D, the destabilization effect appears to be quite weak and may be partially due to the approximation of the 2D grid. In 3D, however, the system is found to be unstable to a ballooning/interchange type of mode with wavenumber ky ρin ∼ 1, where ρin is the ion gyroradius in the normal field. These modes evolve to form intense “heads” of strongly enhanced Bz. In the wake of the heads are regions of strongly reduced or reversed Bz. These local field reversals lead to the onset of reconnection with extremely large electric fields cEy = vTi B0 ∼ 10 that have appreciable electrostatic as well as inductive components. This onset of 3D reconnection appears to be much more intense than in the standard 2D scenario. Instituto Nacional de Pesquisas Espaciais - INPE 42 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T25) ROLE OF RECONNECTION IN ENERGY INPUT FROM SOLAR WIND TO THE MAGNETOSPHERE-IONOSPHERE SYSTEM Tuija I. Pulkkinen[1] [1] Aalto University, Espoo, Finland. e-mail: [email protected] ABSTRACT Pioneering work in space science identified two scenarios by which energy enters from the solar wind into the magnetosphere: Magnetic reconnection and viscous interaction. Observational input-output analyses led to general understanding that reconnection is the dominant process, but even today, there are several competing formulations of the energy coupling function, and the scatter of the results remains large. Quantitative analysis of the GUMICS global MHD simulation results indicate that the electric field component parallel to the large-scale neutral line at the magnetopause gives high correlation as long as the clock angle is away from the purely northward orientation. The simulations further reveal that the IMF and solar wind speed drive the system in different ways, leading to scatter in the input-output analysis using the electric field as the driver function. More scatter is introduced by the effects of fluctuating solar wind and IMF, which also have an effect on the coupling efficiency. We examine the large-scale coupling as a function of the electric field (and hence efficiency of the reconnection process), show the variations arising from electric field dominated by large IMF and by large solar wind speed, and demonstrate the effect of solar wind fluctuations to the ionospheric dissipation. We conclude by estimating the relative contributions of each of the three phenomena. Instituto Nacional de Pesquisas Espaciais - INPE 43 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T26) CURRENT SHEETS FORMATION AND THE HEATING OF SOLAR AND STELLAR CORONAE Franco Rappazzo[1] [1] Bartol Research Institute University of Delaware, USA. e-mail: [email protected] ABSTRACT The convective motions of the outer envelope of all late-type main sequence stars have more than enough energy to sustain the observed atmospheric heating and X-ray emission. These photospheric motions shuffle the footpoints of the magnetic field lines. Parker pointed out that the resulting magnetic field is generally out of equilibrium, and conjectured that the dynamical evolution of almost all interlaced field line topologies leads to the formation of current sheets, corresponding to discontinuities in the ideal limit. The current sheets thickness, their dynamical formation process and associated magnetic reconnection are crucial for the heating process, given the low collisionality of the coronal plasma and the corresponding high value of the magnetic Reynolds number. Dynamics are investigated with dissipative and ideal magnetohydrodynamics models starting with different magnetic field topologies. Their results will be discussed. Instituto Nacional de Pesquisas Espaciais - INPE 44 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T27) IN SITU OBSERVATIONS OF MAGNETIC RECONNECTION IN SOLAR SYSTEM PLASMAS Alessandro Retinò[1] , A. Chasapis, C. Rossi, F. Sahraoui, L. Hadid, A. Vaivads, Y. Khotyaintsev, R. Nakamura, B. Zieger, D. Sundkvist, F. S. Mozer, M. Fujimoto, S. Kasahara, A. Masters, H. Fu [1] Laboratoire de Physique des Plasmas, France. e-mail: [email protected] ABSTRACT Magnetic reconnection is a universal plasma process occurring at current sheets, where smallscale changes in the topology of the magnetic field lead to large-scale plasma transport, heating and acceleration as well as to non-thermal particle acceleration. Reconnection is observed in the solar corona, in the solar wind, in planetary magnetospheres and is considered to play an important role in distant astrophysical objects such as the interstellar medium and accretion disks. Despite of many remote and in-situ observations, however, a number of key issues related to the basic physics of reconnection are still not fully understood. Among them, some of the most important are the microphysics, the mechanisms of non-thermal particle acceleration and the relationship between reconnection and turbulence. Solving such issues from an experimental point of view requires detailed in situ observations of particle distributions functions and electromagnetic fields in reconnection regions. At present, this is only possible in the solar system through spacecraft measurements. Here we review some recent situ observations of reconnection in solar system plasmas, focusing on the problems of the microphysics, particle acceleration and turbulent reconnection. Instituto Nacional de Pesquisas Espaciais - INPE 45 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T28) THE DIAGNOSTIC ROLE OF ELECTRONS IN COLLISIONLESS RECONNECTION1 Jack D. Scudder[1] [1] University of Iowa, USA. e-mail: [email protected] ABSTRACT A program for enhancing the diagnosis of current layers as part of the reconnection site will be discussed that has direct bearing on in situ measurements and 3D PIC simulations when there is no known flux function. The approach is centered on the establishing dimensionless scalar observables that reflect the expected demagnetization of the electrons in the reconnection layer. Spatial collocation of these variables will be shown with theoretical quantities from Maxwell’s equations that may be determined using 3D PIC simulations. 5 dimensionless observables will be introduced that have a strong correlations with quantities related to the curl of the non-ideal electric field and theoretical measures of flux slippage. A general property of these quantities is that they are usually order unity at the reconnection site. The occurrence of smaller enhancements of these scalars occur along separatrices and in other MHD discontinuities or instabilities where they represent much weaker departures from frozen flux than in the vicinity of the electron diffusion region. These examples show that flux slippage in varying degrees is common, but generally not important for the description of such current channels. Thus finding frozen flux violations is not so difficult, but the difficult task is to identify the “important” violations as decisive signatures of the reconnection layer. 1 In collaboration with: W. Daughton, H. Karimabadi and V. Roytershteyn Instituto Nacional de Pesquisas Espaciais - INPE 46 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T29) ANALYTICAL APPROACH IN TIME-DEPENDENT MAGNETIC RECONNECTION OF SKEWED MAGNETIC FIELDS V. S. Semenov[1] [1] University of St. Petersburg. e-mail: [email protected] ABSTRACT An analytical study of set-up, propagation and interaction of non-linear and linear MHD waves driven by reconnection is presented. It is shown how, assuming that the normal component of magnetic field remains small, the structure of the outflow (exhaust) region can be specified in terms of the external parameters in the inflow regions. This non-linear solution of the Riemannian decay of a current sheet serves as a basis for the formulation and solution of the corresponding linear initial-value problem of MHD. It is shown that reconnection of skewed magnetic fields leads to high speed flows inside the exhaust region which is bounded not only by Alfvénic and slow mode waves but also, to a large extent, by tangential discontinuities (TDs). The TD part of the exhaust boundary expands with the distance from the X-line and therefore a long exhaust does not necessarily imply a long X-line. The reconnection rate obtained by the matching of the outer Petschek solution and internal diffusion region solution, incorporates both Sweet-Parker and Petschek regimes, while the latter is possible only for a strongly localized resistivity. Instituto Nacional de Pesquisas Espaciais - INPE 47 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T30) PLASMOID-INDUCED-RECONNECTION AND FRACTAL RECONNECTION IN SOLAR FLARES Kazunari Shibata[1] [1] Kyoto University, Japan. e-mail: [email protected] ABSTRACT Recent space observations of the Sun revealed that magnetic reconnection is ubiquitous in the solar atmosphere, ranging from small scale reconnection (observed as nanoflares) to large scale one (observed as long duration flares or giant arcades). Often these reconnection events are associated with mass ejections or jets, which seem to be closely related to multiple plasmoid ejections from fractal current sheet. Bursty radio and hard X-ray emissions from flares also suggest the fractal reconnection and associated particle acceleration. We would discuss recent observations and theories related to plasmoid-induced-reconnection and fractal reconnection in solar flares, and their implication to reconnection physics and particle acceleration. Instituto Nacional de Pesquisas Espaciais - INPE 48 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T31) SIZE AND SHAPE OF THE DISTANT MAGNETOTAIL David G. Sibeck[1] [1] Goddard Space Flight Center, NASA, USA. e-mail: [email protected] ABSTRACT We employ the BATS-R-US model to study the effects of the interplanetary magnetic field (IMF) strength and orientation upon the cross-section of the magnetotail at lunar distances. The anisotropic pressure of draped magnetosheath magnetic field lines and the inclusion of a reconnection-generated standing slow mode wave fan bounded by a rotational discontinuity within the definition of the magnetotail result in cross-sections elongated in the direction parallel to the component of the IMF in the plane perpendicular to the Sun-Earth line. Tilted cross-tail current sheets separate the northern and southern lobes within these crosssections. Greater fast mode speeds perpendicular than parallel to the draped magnetosheath magnetic field lines result in greater distances to bow shock in the direction perpendicular than parallel to the component of the IMF in the plane perpendicular to the Sun-Earth line. The magnetotail cross-section responds rapidly to variations in the IMF orientation. The rotational discontinuity associated with newly reconnected magnetic field lines requires no more than the magnetosheath convection time to appear at any distance downstream, and further adjustments of the cross-section in response to the anisotropic pressures of the draped magnetic field lines require no more than 10-20 minutes. Consequently for typical ecliptic IMF orientations and strengths, the magnetotail cross-section is oblate while the bow shock is prolate. These predictions are compared with ARTEMIS observations of the magnetotail at lunar distances. Instituto Nacional de Pesquisas Espaciais - INPE 49 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T32) A REVOLUTIONARY AERONOMY CONCEPT TO EXPLORE THE COUPLING OF THE SOLAR-TERRESTRIAL SYSTEM James F. Spann[1] [1] MSFC/NASA, USA. e-mail: [email protected] ABSTRACT A revolutionary opportunity to explore the consequences of reconnection in the ionosphere as never before will be presented. It is a revolutionary opportunity to explore key Aeronomy emissions on a global scale with spatial and temporal resolution not possible today. For example, observations of the signature of dayside merging and nightside reconnection that are reflected in the auroral oval evolution during disturbed periods and quiet times, will be described; observations that will open a window of discovery for coupling phenomena within Geospace and with the solar wind. The description of this new concept will be presented, and its impact and contribution to understanding magnetic merging will be discussed. Instituto Nacional de Pesquisas Espaciais - INPE 50 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T33) KINETIC SIMULATIONS AND THEORY OF WAVE GENERATION AND PARTICLE ACCELERATION AT RECONNECTIONGENERATED DIPOLARIZATION FRONTS Richard D. Sydora[1] , Maha Ashour-Abdalla, Meng Zhou, and Raymond J Walker [1] University of Alberta, Canada. e-mail: [email protected] ABSTRACT Sharp dipolarization fronts (DF’s) can be generated in the outflow regions of magnetic reconnection and are potential sites of sizeable Joule energy dissipation. They are characterized by a strong variation (micro-scale on the order of or less than the ion inertial length, δi = c/ωpi ) and magnitude (Bz /B ∼ 0.5 − 2) of the Earth’s tail magnetic field component Bz , which is normal to the neutral plane [Runov et al., 2009; Sergeev, et al., 2009, Zhou et al., 2009]. Recent THEMIS satellite observations show strong wave activity, particularly in the whistler and lower hybrid frequency range [Deng et al., 2010; Sergeev et al., 2009] as well as electron cyclotron harmonic waves (ECH), up to the upper hybrid frequencies [Zhou et al.,2009]. We focus on these latter high frequency observations and propose a mechanism for ECH excitation based on perpendicular ion beam-driven ECH modes. We have carried out fully electromagnetic particle-in-cell simulations with open boundaries. An Earthward moving DF is initialized in a self-consistent manner at one edge of the simulation domain and followed over distances of approximately 100 ion inertial lengths. The front has a characteristic speed of the local Alfven speed, VA , and the fine scale structure and shape of the DF is strongly dependent on the initial Bz amplitude with non-stationary behavior observed above a threshold in the range Bz /B ∼ 1 − 2. The interface of the DF is characterized by trapped and accelerated ions, thus forming an ion beam component that, through Doppler shifting, couples to the ECH at wavelengths on the electron gyroradius scale. Spectral analysis of the electric field (Ex ) pulse in the direction of propagation, formed by charge separation due to differing particle magnetization, reveals the presence of non-thermal ECH waves with maximum field energy near the upper hybrid mode frequency. These physical processes appear consistent with detailed analysis of a particular THEMIS event on Feb. 15, 2008 in the near-Earth region [Zhou et al., 2009]. Instituto Nacional de Pesquisas Espaciais - INPE 51 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T34) ASSESSING THE VALIDITY OF THE MAXIMUM MAGNETIC SHEAR MODEL: A REVIEW Karlheinz J. Trattner[1] [1] University of Colorado, LASP, Boulder, USA. e-mail: [email protected] ABSTRACT Reconnection at the Earth’s magnetopause is the mechanism by which magnetic fields in different regions change topology to create open magnetic field lines that allow energy and momentum to flow into the magnetosphere. One of the long standing questions about magnetic reconnection is the location of the reconnection line. There are two reconnection scenarios discussed in the literature: a) anti-parallel reconnection where shear angles between the magnetospheric field and the interplanetary magnetic field (IMF) are near 180◦ , and b) component reconnection where a tilted reconnection line which crosses the magnetopause in the sub-solar region at shear angles not near 180◦ . Early satellite observations were limited to the detection of accelerated ion beams in the magnetopause boundary layer to determine the general direction of the reconnection line location with respect to the satellite. An improved view of the reconnection location at the magnetopause was determined from ionospheric emissions observed by polar-orbiting imagers which revealed that both scenarios occur. The time-of-flight effect of precipitating ions in the cusp in connection with the low-velocity cutoff method pin-pointed reconnection locations and their dependency on IMF conditions. These results are summarized by the Maximum Magnetic Shear Model. This review will discuss several studies which compared their observations to the predictions of the Maximum Magnetic Shear model. The results reveal that the Maximum Magnetic Shear model predicts the observed reconnection locations for dominant IMF BY conditions very well, but needs modifications for dominant southward IMF conditions. Instituto Nacional de Pesquisas Espaciais - INPE 52 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T35) FLUID AND KINETIC SIGNATURES OF RECONNECTION AT THE DAYSIDE MAGNETOPAUSE OBSERVED BY DOUBLE STAR TC1 Lorenzo Trenchi[1] [1] IFSI-National Institute for Astrophysics, Italy. e-mail: [email protected] ABSTRACT Magnetic reconnection is probably the main process which allows the solar wind entry into the Earth’s Magnetopause. Several studies from satellite and ground based observations confirm this hypothesis. However, many questions are still open as the ones regarding the influence of boundary conditions. In this talk we present a statistical study of magnetic reconnection at the dayside magnetopause based on Double Star TC1 data. The Walén relation is used to identify the reconnection events and the occurrence of reconnection jets, in relation to various magnetosheath parameters, is investigated. These observations indicate the presence of a reconnection line hinged near the subsolar point and tilted according to the observed magnetosheath clock angle, consistently with the component merging model. The detailed study of the ion distribution functions observed during the reconnection jets is performed. The Kinetic signatures of magnetic reconnection are based on the D-shaped distributions of transmitted magnetosheath ions in the boundary layer, with a parallel velocity cutoff at the deHoffmann-Teller velocity. These D-shaped distributions are not found at all the magnetopause crossings which satisfy Walén relation. Here we present the occurrence of the D-shaped distributions in relation to the different plasma conditions characterizing each crossing and give evidence of the importance of the velocity shear and magnetic field shear angle in the mutual occurrence of fluid and kinetic signatures of reconnection. Instituto Nacional de Pesquisas Espaciais - INPE 53 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T36) RADIATIVE MAGNETIC RECONNECTION IN ASTRO- PHYSICS Dmitri Uzdensky[1] [1] CIPS, University of Colorado, Boulder, USA. e-mail: [email protected] ABSTRACT Historically, traditional magnetic reconnection has focused on relatively tenuous solar-system environments, where radiation can be ignored. In contrast, in many astrophysical situations the energy density in the reconnection region is so high that radiation becomes important. I will give an overview of recent progress on radiative astrophysical magnetic reconnection — a new frontier in plasma astrophysics. I will outline the most important radiative effects that may influence reconnection dynamics and particle acceleration: radiative cooling, radiation pressure, and Compton drag resistivity. I will illustrate these radiative aspects of reconnection with specific astrophysical examples, including magnetar flares; accretion-disk coronae; reconnection powering high-energy emission in pulsar magnetospheres; and recently discovered gamma-ray flares in the Crab Nebula. Finally, I will present a generalization of the resistive-MHD Sweet-Parker reconnection model to the strong radiative cooling case. Instituto Nacional de Pesquisas Espaciais - INPE 54 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T37) THE AXFORD CONJECTURE AND THE PROPERTIES OF AN OPEN MAGNETOSPHERE Vytenis M. Vasyliunas[1] [1] Max Planck Institute, Germany. e-mail: [email protected] ABSTRACT Magnetic reconnection can occur only if there are departures from ideal MHD. An obvious question is the extent to which the parameters specifying the non-MHD effects (electrical resistivity, inertial length, gyroradius, etc.) influence the configuration of the system. This question is often stated as: what determines the reconnection rate? A more specific formulation, applied to a particular system (e.g., the Earth’s magnetosphere) is: what determines the amount of open magnetic flux and the rate of magnetic flux transport? These quantitative global parameters can be empirically estimated (from polar-cap area and from cross-polarcap potential, respectively, among other methods) and have with some success been related to solar-wind parameters. The concept that such global parameters are determined primarily by large-scale MHD dynamics and boundary conditions, with non-MHD effects important mostly for determining properties of local small-scale structures such as boundary layers, was persistently and eloquently argued especially by W.I. Axford and is often called the “Axford conjecture.” Recent criticisms of the conjecture are based to a large extent on a misunderstanding of what it means. Unless the Axford conjecture is assumed to be valid at least to some degree of approximation, global MHD simulations of the magnetosphere (most of which do not even pretend to model non-MHD effects adequately) cannot be trusted to give reliable results on anything related to reconnection. Attempts to understand from first principles and derive theoretically the empirically established relations between the solar wind and the global properties of the open magnetosphere (or their proxies in geomagnetic/magnetospheric indices) require careful consideration of the Axford conjecture and related basic assumptions. Instituto Nacional de Pesquisas Espaciais - INPE 55 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T38) SIMULATION STUDIES OF PLASMA TRANSPORT AT THE EARTH AND OUTER PLANETS Raymond J. Walker[1] , Keiichiro Fukazawa, and Tatsuki Ogino [1] IGPP, University of California, Los Angeles, USA. e-mail: [email protected] ABSTRACT We have used a three-dimensional magnetohydrodynamic simulation code to model the magnetospheres of the Earth, Jupiter and Saturn. At the Earth reconnection between the interplanetary magnetic field (IMF) and magnetosphere dominates magnetospheric transport. At the rapid rotating planets, Jupiter and Saturn, that reconnection occurs is evidenced by their long magnetotails with open magnetic flux. However transport is dominated by planetary driven rotation. In particular reconnection has relatively little effect at Saturn. At Saturn flow shear instabilities like the Kelvin-Helmholtz instability become important for driving transport. Instituto Nacional de Pesquisas Espaciais - INPE 56 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T39) PARALLEL ELECTRIC FIELDS AND SUBCAVITIES IN MAGNETOTAIL RECONNECTION (ASSUMED TITLE) Rongsheng Wang[1] [1] Geophysical Institute, Chinese Academy of Sciences, Beijing, China. e-mail: [email protected] ABSTRACT We investigate a direct south-north crossing of a reconnection ion diffusion region in the magnetotail. During this crossing, multiple electron density dips with a further density decrease within the cavity, called subcavities, adjacent to the northern separatrix are observed. The correlation between electron density sub-cavities and strong electric field fluctuations is obvious. Within one of the sub-cavities, a series of very strong oscillating perpendicular electric field and patchy parallel electric field are observed. The parallel electric field is nearly unipolar and directs away from X line. In the same region, inflow electrons with energy up to 100 keV are injected into the X line. Based on the observations, we conclude that the higher energy inflowing electrons are accelerated by the patchy parallel electric field. Namely, electrons have been effectively accelerated while they are flowing into the X line along the separatrix. The observations indicate that the electron acceleration region is widely larger than the predicted electron diffusion region in the classical Hall magnetic reconnection model Instituto Nacional de Pesquisas Espaciais - INPE 57 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T40) STUDY OF PARTICLE ENERGIZATION DURING MAGNETIC RECONNECTION IN A LABORATORY PLASMA2 Masaaki Yamada[1] [1] Princeton Plasma Physics Laboratory, USA. e-mail: [email protected] ABSTRACT One of the most important outstanding issues in magnetic reconnection is how the energy of reconnecting magnetic field is converted to the kinetic energy of ions and electrons. Quantitative Study of the energization of plasma particles in the magnetic reconnection layer has been carried out by monitoring the behavior of electrons and ions in MRX (1, 2). The measured profiles of plasma parameters are quantitatively analyzed with symmetric as well as asymmetric upstream conditions in the context of the two-fluid reconnection physics (1) and compared with the recent numerical simulation results. The electron heating is observed to extend beyond the electron diffusion region and considered to be due to energization by magnetic instabilities of incoming electrons trapped in the magnetic mirror. This energization often occurs impulsively. Ions are accelerated by an electrostatic field across the separatrices to the plasma exhaust region of the reconnection layer and become thermalized through re-magnetization by the exiting magnetic fields. In this paper, the acceleration and heating of ions and electrons which extents much larger than the length scale of the ion skin depth, is addressed quantitatively for the first time in a laboratory reconnection layer. A total energy inventory is calculated based on analysis of the Poynting vector, enthalpy, flow energy, and heat flux in the measured diffusion layer (3). More than a half of the incoming magnetic energy is converted to particle energy during collisionless reconnection. The results will bring a new insight into the conversion mechanism of magnetic energy to that of plasma particles during magnetic reconnection. (1) M. Yamada, R. Kulsrud, H. Ji, Rev. Mod. Phys. v.82, 602 (2010) (2) J. Yoo et al, Phys. Rev. Letts. 110, 215007 (2013) (3) J. Eastwood et al., PRL 110, 225001 (2013) 2 In collaboration with J. Yoo, and C. Swanson, J. Jara Almonte, H. Ji, C. Myers, PPPL, Princeton University, Li-Jen Chen, University of New Hampshire. Instituto Nacional de Pesquisas Espaciais - INPE 58 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T41) THE STRUCTURE OF THE DIFFUSION REGION IN COLLISIONLESS RECONNECTION: THEORY, SIMULATION, AND OBSERVATION Seiji Zenitani[1] [1] National Astronomical Observatory of Japan, Japan. e-mail: [email protected] ABSTRACT The structure of the diffusion region is of strong interest in reconnection physics. Earlier expectations agree that it has a multi-scale structure, an outer layer in which ions decouple from the magnetic field and an inner layer in which electrons are unmagnetized. They are popularly called “electron diffusion (dissipation) region“ or ”ion diffusion region“, but recent particlein-cell (PIC) simulations have revealed a complicated picture. In this talk, we overview our recent attempts to better understand these structures in collisionless reconnection. First, we review several fundamental notions such the magnetic dissipation and the magnetic diffusion. Particular attention will be paid to their relevance to the plasma ideal condition. Then we evaluate the kinetic structure near the X-line in two-dimensional PIC simulations. We will also review our Geotail observation of the reconnection site in the magnetotail. Instituto Nacional de Pesquisas Espaciais - INPE 59 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T42) THE ROLE OF MAGNETIC RECONNECTION ON COSMIC RAY ACCELERATION Elizabete de Gouveia Dal Pino[1] [1] Universidade de São Paulo, Instituto de Astronomia, Geofı́sica e Ciências Atmosféricas, USP, IAG, SP, Brazil. e-mail: [email protected] ABSTRACT Cosmic Ray acceleration still challenges the researchers. Cosmic rays may be accelerated in astrophysical environments by a variety of processes. Acceleration in magnetic reconnection sites, in particular, has lately attracted the attention of researchers not only for its potential importance in the solar system context, but also in other astrophysical environments, like black hole binaries (microquasars), AGNs and GRBs, and even in diffusive media like the ISM and the IGM, in order to explain new puzzling high energy observations. In this talk we review this process and present three-dimensional MHD simulations with the injection of thousands of test particles and show from the evolution of their energy spectrum that they are efficiently accelerated by reconnection through a first-order Fermi process within large scale magnetic current sheets, as predicted by de Gouveia Dal Pino and Lazarian in 2005 (particularly when local turbulence is present, making reconnection fast and the acceleration region thicker). We will also show that the magnetic power released by fast magnetic reconnection in compact sources is more than sufficient to accelerate relativistic plasmons and produce the observed radio (and gamma ray) luminosity in microquasars and low luminous AGNs. Furthermore, this process can naturally explain the observed correlation between the radio luminosity and the mass of these sources spanning 109 orders of magnitude (namely, the so-called fundamental plane). Instituto Nacional de Pesquisas Espaciais - INPE 60 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T43) ANALYSIS OF SOLAR FLARES FROM MICROWAVES TO THz FREQUENCIES AND CHALLENGES FOR INTERPRETATION Pierre Kauffmann[1] [1] Universidade Presbiteriana Mackenzie, São Paulo, SP, Brazil. e-mail: [email protected] ABSTRACT A number of solar bursts have been observed to have unexpected distinct spectral components in the GHz to sub-THz range: one corresponds to the well known microwaves emission maximizing at few to tens GHz, and another with fluxes increasing again for larger sub-THz frequencies. Recently a dramatic double-spectral structure feature was observed during an intense 30 THz impulsive burst with flux several times larger than the microwave component. These results raise serious problems to explain the simultaneous presence of the sub-THz and the concurrent microwave component. Authors have suggested explanations for the sub-THz spectral component include emission by free-free collisions of thermal electrons, synchrotron produced by high energy electrons; emission by Langmuir waves excited by beams of electrons and protons at denser regions of the solar active centers and inverse-Compton effect on the field of synchrotron electrons; inverse-Compton effect on field of photons produced by Langmuir waves and the Vavilov-Cherenkov emission by high energy electrons on an assumed partially ionized chromospheric gas. More than one mechanism might be acting at the same time and that a free-free contribution might always be present to a certain level. Most explanations used to explain the sub-THz spectral component do not account for the concurrent microwaves spectral component that is also observed. One possibility is that both spectral components can be produced by a single beam of high energy electrons undergoing processes similar to those occurring in laboratory accelerators. Incoherent synchrotron radiation (ISR) is produced by a beam of very high energy electrons (> MeVs) with flux maximizing somewhere on the THz range of frequencies. On the other hand physical perturbations may produce multiple electrons closely in phase at microbunches in the electron beams, which could emit broadband coherent synchrotron radiation (CSR) in the GHz range of frequencies and thus bringing a simultaneous contribution to the low frequency spectral component. To improve our understanding of the physical processes involved it is necessary to obtain a more complete spectral description of emissions from microwaves to THz frequencies. Instituto Nacional de Pesquisas Espaciais - INPE 61 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T44) FAST MAGNETIC RECONNECTION IN TURBULENT MEDIA Grzegorz Kowal[1] [1] Escola de Artes, Ciências e Humanidades (EACH), São Paulo, SP, Brazil. e-mail: [email protected] ABSTRACT In this talk I will present the results of our numerical studies on a model of fast magnetic reconnection in the presence of weak turbulence proposed by Lazarian and Vishniac (1999). The three-dimensional direct numerical simulations show that the reconnection of magnetic field becomes fast, i.e. independent of resistivity, in the presence of weak turbulence in the way consistent with the Lazarian and Vishniac (1999) model. I will discuss our results on the reconnection rate scalings, independence of the way of the turbulence injection happens, the ability of reconnection to generate turbulence and therefore self-sustains its fast rate, as well demonstrate that the process of reconnection is an efficient particle accelerator producing cosmic rays through the first order Fermi process. Instituto Nacional de Pesquisas Espaciais - INPE 62 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil T45) ANNIHILATION OF QUANTUM MAGNETIC FLUXES IN SUPERCONDUCTING SYSTEMS AND NEUTRON STARS Walter D. Gonzalez[1] [1] Geophysics Division/CEA - INPE , São José dos Campos, SP, Brazil. e-mail: [email protected] ABSTRACT After discussing the implications of the Aharonov and Bohm effect on the existence of a quantum of magnetic flux (QMF), I will describe the Ginzburg-Landau theory that explains its origin and show some observations of QMFs obtained in the laboratory using superconducting systems. Then, I will discuss the processes related with the annihilation of QMFs of opposite directions (vortices and antivortices ) which may result in the emission of photons in the UV and soft x-ray range for magnetic fields of 1-100 Gauss. Finally, I will mention an application of these concepts to the possible emission of intense gamma rays from accreting neutron star cores. Instituto Nacional de Pesquisas Espaciais - INPE 63 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 4.2 Poster Contribution Abstracts Instituto Nacional de Pesquisas Espaciais - INPE 64 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P1) ENERGETIC PROTONS CROSS-FIELD DIFFUSION IN THE HELIOSPHERE Edio da Costa Junior[1] , Bruce T. Tsurutani[2] , Maria Virgı́nia Alves[3] , Ezequiel Echer[3] and Gurbax S. Lakhina[4] [1] Instituto Federal de Minas Gerais-IFMG, Ouro Preto, MG, 35400-000, Brazil. e-mail: [email protected] [2] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA [3] Instituto Nacional de Pesquisas Espaciais-INPE, São José dos Campos, SP, 12227-010, Brazil [4] Indian Institute for Geomagnetism, Navi Mumbai 410 218, India ABSTRACT Magnetic field magnitude decreases (MDs) are observed in several regions of the interplanetary medium. In this work, we characterize MDs observed by the Ulysses spacecraft instrumentation over the solar south pole by using magnetic field data to obtain the empirical size, magnetic field MD, and frequency of occurrence distribution functions. The interaction of energetic (100 keV to 2 MeV) protons with these MDs is investigated. Charged particle and MD interactions can be described by a geometrical model allowing the calculation of the guiding center shift after each interaction. Using the distribution functions for the MD characteristics, Monte Carlo simulations are used to obtain the cross-field diffusion coefficients as a function of particle kinetic energy. It is found that the protons under consideration cross-field diffuse at a rate of up to ≈ 11% of the Bohm rate. The same method used here can be applied to other space regions where MDs are observed, once their local features are well known. Instituto Nacional de Pesquisas Espaciais - INPE 65 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P2) SOLAR MEAN FLOWS AND DYNAMO, A CRITICAL, UPDATED, REVIEW Gustavo Guerrero[1] [1] Department of Physics, Federal University of Minas Gerais, Belo Horizonte, MG, Brazil. e-mail: [email protected] ABSTRACT One of the most important contributions of Professor Parker to solar physics was the proposal of the turbulent dynamo mechanism to explain the 11-year sunspot cycle. Even though his theory was formulated more than 50 years ago and several models have been proposed ever since, his ideas remain extremely recent. Observational evidence seems to indicate to us that the dynamo operating in the Sun should be of the alpha-omega type. Being alpha the contribution of helical turbulence and Omega the inductive action of differential rotation. As a matter of fact, differential rotation (and meridional circulation) also results from collective turbulent effects. So turbulence is the key ingredient in solar activity modelling. In this talk I will review the recent advances in the modeling of solar mean-flows and dynamo. I will discuss the pros and cons of mean field models (which parametrize the turbulent contribution) as well as of the most recent approach, i.e., 3D MHD dynamical models in a spherical geometry. Instituto Nacional de Pesquisas Espaciais - INPE 66 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P3) SOLAR FLARES OBSERVED WITH POEMAS Adriana Válio[1] , P. Kaufmann[1] , C. Guillermo Giménez de Castro[1] [1] CRAAM, Universidade Presbiteriana Mackenzie, Brazil. e-mail: [email protected] ABSTRACT POEMAS (POlarization Emission of Millimeter Activity at the Sun) is a new system of two circular polarization solar radio telescopes for observations of the Sun at 45 and 90 GHz. The novel characteristic of these instruments is the capability to measure circular right- and lefthand polarizations at these high frequencies. The two frequencies were chosen so as to bridge the gap at radio frequencies between 20 and 200 GHz of solar flare spectra. The telescope system saw first light in November 2011 and is satisfactorily operating daily since then. Here we present the observation of a few flares detected by the telescopes. The millimeter spectra of some flares are seen to rise toward higher frequencies, indicating the presence of a new spectral component distinct from the microwave one. Instituto Nacional de Pesquisas Espaciais - INPE 67 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P4) STATISTICAL ANALYSIS OF RADAR OBSERVED F REGION IRREGULARITIES FROM THREE LONGITUDINAL SECTORS R. Y. C. Cueva[1,2] , E. R. de Paula[1] and A. E. Kherani[1] [1] Aeronomy Division, DAE, National Institute for Space Research (INPE), São José dos Campos, 12227-010, São Paulo, Brazil. e-mail: [email protected] [2] Centro de Radio Astronomia e Astrofı́sica Mackenzie, CRAAM, Presbyterian Mackenzie University, São Paulo, Brazil ABSTRACT Equatorial Spread F (ESF) is a manifestation of ionospheric interchange instabilities in the nighttime equatorial F region. These instabilities generate plasma density irregularities with scale sizes ranging from centimetres to thousands of kilometres. The irregularities can be detected from a variety of instruments such as digisonde, coherent and incoherent scatter radars, in situ space probes, and airglow photometers. In the present study, occurrence statistics of the ESF, based on various parameters are presented using data obtained from the VHF radars located at three longitudinally separated equatorial stations: Christmas Island (2 N, 202.6 E, 2.9 N dip latitude), São Luı́s (2.59 S, 315.8 E, 0.5 S dip latitude) and Jicamarca (12 S, 283.1 E, 0.6 N dip latitude). The ESF parameters presented here are the onset altitude, onset time (onset refers to first appearance of signal in the radar field of view) of the bottom-type and plume, and the peak altitude of the plume. Recent studies have used these parameters to classify the spread F occurrence characteristics. The present study reveals novel features namely, the dependence of ESF parameters on the seasonal, solar flux, declination angle and longitudinal dependence from the three radar sites. In addition, we also present an empirical model to determine the nature of these ESF parameters as a function of the solar flux which may enable us to forecast (with 30 min to 1 h tolerance) the plume occurrence at any longitude located in between São Luı́s and Christmas Island. Instituto Nacional de Pesquisas Espaciais - INPE 68 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P5) MAGNETOPAUSE RECONNECTION AND INTERLINKED FLUX TUBES F. R. Cardoso[1] , W. D. Gonzalez[2] , D. G. Sibeck[3] , M. Kuznetsova[3] , and D. Koga[2] [1] EEL/USP - Escola de Engenharia de Lorena/ Universidade de São Paulo, Lorena, São Paulo, Brazil. e-mail: [email protected] [2] INPE - Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, Brazil [3] NASA Goddard Space Flight Center, Greenbelt, MD, USA ABSTRACT Magnetic reconnection can be a continuous or a transient process. Global magnetohydrodynamics (MHD) simulations are important tools to understand the relevant magnetic reconnection mechanisms and the resulting magnetic structures. We have studied magnetopause reconnection using a global 3-D MHD simulation in which the interplanetary magnetic field (IMF) has been set to large positive By and large negative Bz components, i.e., a southduskward direction. Flux tubes have been observed even during these constant solar wind conditions. We have focused on the interlinked flux tubes event resulting from time-dependent, patchy and multiple reconnection. At the event onset, two reconnection modes seem to occur simultaneously: a time dependent,patchy and multiple reconnection for the subsolar region; and, a steady and large-scale reconnection for the regions far from the subsolar site. Instituto Nacional de Pesquisas Espaciais - INPE 69 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P6) TRANSPORT BARRIERS IN CONFINED PLASMAS Iberê Luiz Caldas[1] [1] Institute of Physics, University of São Paulo, São Paulo, Brazil. e-mail: [email protected] ABSTRACT Initially, we show how transport barriers are created in nonmonotonic dynamical systems. These barriers reduce the transport in the shearless region (i.e., where the twist condition does not hold). Then, we analyze two kinds of problems in plasma with non-monotonic field profiles: the first is the chaotic magnetic field line transport in plasmas with external resonant perturbations; the second problem is the chaotic particle drift motion caused by electrostatic waves. Thus, initially, we consider chaotic magnetic field lines, in the region near a tokamak wall, with resonant modes due to electric currents in external coils. For nonmonotonic plasma electric current density profiles, we obtain distributions of field line connections to the wall and line escape channels with the same spatial pattern as the magnetic footprints on the tokamak walls [1]. Furthermore, considering the chaotic particle transport in equilibrium electric fields with a nonmonotonic radial profile perturbed by electrostatic waves, we present evidences of nontwist transport barriers at the plasma edge tokamak [2] and in helimaks [3]. 1- Escape Patterns of Chaotic Magnetic Field Lines in a Tokamak with Reversed Magnetic Shear and an Ergodic Limiter. T. Kroetz, M. Roberto, E. C. Silva, I. L. Caldas, R. L. Viana. Phys. Plasmas 15, 092310 (2008). 2- Reduction of Chaotic Particle Transport Driven by Drift Waves in Sheared Flows. A. F. Marcus, I. L. Caldas, Z. O. Guimarães-Filho, P. J. Morrison, W. Horton, I. C. Nascimento, Yu. K. Kuznetsov. Phys. Plasmas 15, 112304 (2008). 3- Turbulence driven particle transport in Texas Helimak. D. L. Toufen, Z. O. GuimarãesFilho, I. L. Caldas, F. A. Marcus, K. W. Gentle. Phys. Plasmas (2012). Instituto Nacional de Pesquisas Espaciais - INPE 70 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P7) THE ROLE OF MAGNETIC ACTIVITY AND RECONNECTION ON THE RADIO AND GAMMA-RAY EMISSION OF COMPACT SOURCES Luı́s H.S. Kadowaki[1] , and Elisabete M. de Gouveia Dal Pino[2] [1] University of São Paulo (IAG-USP), São Paulo, Brazil. e-mail: [email protected] ABSTRACT Fast magnetic reconnection events can be a very powerful mechanism operating at the jet launching region of compact sources such as microquasars and AGNs. It has been found that the power released by reconnection between the magnetic field lines of the coronal inner disk region and the lines anchored into the black hole of these sources is able to accelerate relativistic particles through a first-order Fermi process and produce the observed radio luminosity from both microquasars and low luminosity AGNs (LLAGNs). Further, the observed correlation between the radio luminosity and the mass of these sources, spanning 109 orders of magnitude in mass, is naturally explained by this process (de Gouveia Dal Pino, Piovezan, Kadowaki 2010). In the present work, assuming that the gamma-ray emission from these sources is probably originated in the same acceleration zones that produce the radio emission, we have applied the scenario above to an extensive number of sources including high luminosity AGNs (HLAGNs) and LLAGNs, microquasars and GRBs. We find that the magnetic reconnection power is sufficient to explain, besides the radio, also the gamma-emission from microquasars (Cgy-X1 and Cgy-X3) and at least from one LLAGN (the radio-galaxy M87) while neither the radio nor the gamma emission from the HLAGNs (Blazars) or from GRBs is fitted by the model. We attribute the lack of correlation of the gamma emission for most of the LLAGNs to the fact that this processed emission does not depend only on the local magnetic field activity around the source/accretion disk, but also on other environmental factors like the photon and density fields. We conclude that the gamma emission we see from microquasars can come from the nuclear region of the sources and be driven by primary relativistic particles accelerated by fast magnetic reconnection events. However, in the case of the HLAGNs (and also, as expected, of GRBs), any nuclear radio or gamma emission is screened by the surrounding density and photon fields of the relativistic jet and therefore, what is observed is only the emission produced further out in the ejecta. Instituto Nacional de Pesquisas Espaciais - INPE 71 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P8) A MAGNETIC RECONNECTION MODEL FOR EXPLAINING AGNs AND MICROQUASARS RADIATION B. Khiali[1] , E.M. de Gouveia Dal Pino[1] , M. V. del Valle[2] , G. Kowal[1] , H. Sol[3] [1] University of São Paulo (IAG-USP, Brazil). e-mail: [email protected] [2] IAR, CONICET, Argentina [3] Observatoire de Meudon, France ABSTRACT Very high energy observations of AGNs are challenging current theories of particle acceleration (mostly based on shock acceleration) which have to explain how particles are accelerated to energies above TeV in very compact regions compared to the characteristic scales of their sources. The identification of microquasars and AGNs as sites of particle acceleration raises many fascinating and important questions. Recent magneto-hydrodynamical studies have revealed that cosmic ray acceleration by fast magnetic reconnection can be rather efficient because a first-order Fermi process may occur. In this work, we discuss this acceleration mechanism in the coronal region of the accretion disk around microquasars and AGNs. In addition, the accelerated particles lose substantial amounts of their energy due to non-thermal interactions with the surrounding magnetic field, matter and radiation fields. We will compute the corresponding acceleration rate and the relevant loss rates in order to reproduce the observed spectral energy distribution for a number of AGNs and microquasars (e.g., M87, Cyg-X1, Cyg-X3, etc), considering the model above and leptonic and hadronic processes. Instituto Nacional de Pesquisas Espaciais - INPE 72 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P9) SPECTRUM OF ELECTROMAGNETIC WAVES OBTAINED AS ASYMPTOTIC QUASI-EQUILIBRIUM SOLUTION OF THE EQUATIONS OF THE THEORY OF WEAK TURBULENCE IN UNMAGNETIZED PLASMAS L. F. Ziebell[1] , Peter H. Yoon[2,3] , R. Gaelzer[1] , J. Pavan[4] , and F. J. R. Simões Jr.[4] [1] Instituto de Fı́sica, UFRGS, Caixa Postal 15051, 91501-970 Porto Alegre, RS, Brazil. e-mail: [email protected] [2] School of Space Research, Kyung Hee University, Yongin, Gyeonggi 446-701, Korea [3] Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, U.S.A. [4] Instituto de Fı́sica e Matemática, UFPel, Caixa Postal 354, 96010-900 Pelotas, RS, Brazil ABSTRACT We consider the equations of the theory of weak turbulence in unmagnetized plasmas, including effects of spontaneous and induced emission, three-wave decay and scattering, and discuss the possibility of generation of electromagnetic waves as a consequence of the existence of a thermal population of plasma particles, without requiring the presence of a particle beam. The conventional belief, based on standard applications of weak turbulence theory, is that the electromagnetic mode can only be excited by nonlinear wave-wave interaction, as the result of coalescence of Langmuir and ion-acoustic waves excited by a beam-plasma instability. In the proposed scenario, the spectrum of electromagnetic waves is generated by nonlinear processes and can be described as a turbulent quasi-equilibrium state which is a natural consequence of the existence of thermal fluctuations. Assuming initial velocity distributions for the plasma particles, spectra of Langmuir and ion-acoustic waves can be obtained, which satisfy the condition of equilibrium between spontaneous and induced emission. As a consequence of the equilibrium spectra of electrostatic waves and of the occurrence of nonlinear interaction between waves and between waves and particles, transverse waves are generated. We show some results of numerical analysis of the system of weak turbulence equations, considering a two-dimensional approximation, which display the early stages of the evolution of the spectrum of transverse waves, and then obtain an analytical asymptotic solution assuming three dimensional situation with azimuthal symmetry. Some results obtained with a particle-in-cell Instituto Nacional de Pesquisas Espaciais - INPE 73 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil simulation code are also shown, and give support to the results originated from the weak turbulence analysis. Instituto Nacional de Pesquisas Espaciais - INPE 74 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P10) TEMPERATURE-ANISOTROPY-DRIVEN INSTABILITIES GENERATED BY THE SUPERTHERMAL DISTRIBUTIONS OBSERVED IN THE SOLAR WIND R. Gaelzer[1] , L. F. Ziebell[1] , and M. S. dos Santos[1] [1] Instituto de Fı́sica, UFRGS, Caixa Postal 15051, 91501-970 Porto Alegre, RS, Brazil. e-mail: [email protected] ABSTRACT In recent years, the effects of particle distribution functions that exhibit a power-law (i. e., non- Maxwellian) dependence on the high-energy tail have attracted several studies by the space plasma community. Such functions, usually known as superthermal or kappa distributions, have been found to provide a better fitting to the velocity distribution functions (VDF) measured by several spacecraft in the plasma environment of the solar wind. Combinations of kappa distributions have been used to model both the electrons and the positive ions that populate the solar wind, and the results obtained from such VDF are constantly adding to, or modifying, the established understanding on the physical processes that take place on the noncollisional and highly asymmetric plasma of the solar wind. One of the problems that is being addressed on this new light is the temperature anisotropy displayed by solar wind protons on the vicinity of Earth’s foreshock. The FDV observed by several spacecraft show nonthermal features such as a very anisotropic core, an extended high-energy tail and a beam population, aligned to the local magnetic field and separated from the core by speeds on the order of the Alfvén speed. The existence of these nonthermal characteristics means that the proton VDF contains a large amount of free energy that can be used to excite and interact with the Alfvén waves present in the solar wind. Conversely, the wave-particle interaction is an important factor that determine the shapes of the VDF observed by the spacecraft. The temperature anisotropy displayed by the solar wind protons around the foreshock extends over a large range of values of the parallel beta parameter, but shows clear boundaries that are evidently related to temperature-anisotropy instabilities such as the mirror, ion-cyclotron and firehose instabilities. However, the stability criteria for these instabilities, as derived from the standard plasma kinetic theory, have not been able to adequately explain the observed anisotropies. One of the alternate theories that have been pursued in the recent years proposes that one must employ superthermal FDV, instead of the usual combination of Maxwellians, in order to adequately model the plasma in the solar wind. In this work, we employ two different models for anisotropic kappa distributions that can be found in the literature and Instituto Nacional de Pesquisas Espaciais - INPE 75 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil compare the dispersion characteristics and growth rates predicted from each one and the eventual effect on the temperature anisotropy allowed for the protons that can match the results obtained. Instituto Nacional de Pesquisas Espaciais - INPE 76 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P11) PIC SIMULATIONS OF ELECTROSTATIC HARMONIC EMISSIONS IN SPACE PLASMAS F. C. H. Machado[1] , F. J. R. Simões Jr.[1] , M. V. Alves[2] [1] Dep. de Fı́sica, UFPel, Pelotas, RS, Brazil. e-mail: [email protected] [2] Divisão de Geofı́sica Espacial, INPE, S. J. dos Campos, SP, Brazil ABSTRACT In this paper, an electromagnetic particle code is used to investigate the electrostatic harmonic emissions as a result of the non-linear interaction of multiple electron beams with a background plasma. Specifically, we perform particle-in-cell simulations to investigate the effect of different beam plasma density ratios as well beam plasma velocity ratios on the multiple harmonic emissions. Our results show that after the injection of the second electron beam into the system the harmonics of electrostatic plasma waves are shifted to low frequencies in the ω × k diagram. This dynamic occurs until a certain limit when the plasma frequency of the second electron beam is close to the electron plasma frequency of the first beam and the harmonics are suppressed. Instituto Nacional de Pesquisas Espaciais - INPE 77 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P12) UNIVERSAL SCALING LAWS FOR FULLY-DEVELOPED MAGNETIC FIELD TURBULENCE NEAR AND FAR UPSTREAM OF THE EARTH’S BOW SHOCK Rodrigo A. Miranda[1] , Abraham C.-L. Chian[2,4] , and Erico L. Rempel[3,4] [1] University of Brası́lia (UnB), Faculty UnB-Gama, and Plasma Physics Laboratory, Institute of Physics, Brası́lia-DF, 70910-900, Brazil. e-mail: [email protected] [2] Observatoire de Paris, LESIA, CNRS, 92195 Meudon, France [3] Institute of Aeronautical Technology (ITA), São José dos Campos-SP 12228-900, Brazil [4] National Institute for Space Research (INPE), São José dos Campos-SP 12227010, Brazil ABSTRACT The power spectrum of magnetic field fluctuations in the interplanetary solar wind displays an inertial subrange with power-law scaling where the spectral index is nearly -5/3, which is indicative of a turbulent state. The turbulent magnetic field displays probability distribution functions that become non-Gaussian with decreasing scale and strong departures from self-similarity and monofractality. The scale dependence of magnetic field fluctuations is due to the presence of rare, large-amplitude coherent structures that dominate the statistics of fluctuations at small scales. We analyze the multifractal scaling of the modulus of the interplanetary magnetic field near and far upstream of the Earth’s bow shock, measured by Cluster and ACE, respectively, from 1 to 3 February 2002. The maximum order of the structure function is carefully estimated for each time series using two independent techniques. The first technique consists of plotting the integrand of the p-th order structure function, and the second technique is a quantitative method which relies on the power-law scaling of the extreme events. We compare the scaling exponents computed from the structure functions of magnetic field differences with the predictions obtained by the She-Lévêque model of intermittency in anisotropic magnetohydrodynamic turbulence. Our results render support for the modelling of universal scaling laws based on the Kolmogorov phenomenology in the presence of sheet-like dissipative structures. Instituto Nacional de Pesquisas Espaciais - INPE 78 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P13) A PLASMA THRUSTER BASED ON AURORA TYPE PARTICLE ACCELERATION MECHANISMS José Leonardo Ferreira[1] , Artur Castelo Branco Santos Serra[1] , and Aderson Lucas Medeiros[1] [1] Plasma Physics Laboratory, University of Brasilia 70910-900 Brası́lia-DF, Brazil. e-mail: [email protected] ABSTRACT This work describes efforts and the work done to construct and develop the first brazillian AURORAL PLASMA THRUSTER. Plasma expanding along diverging magnetic Field lines generate a current free Double layer, which potential drop accelerates the ions, forming a supersonic ion beam, useful for high specific impulse thrusting. Typically, the plasma is generated by a helicon discharge in a region of uniform axial magnetic field that is connected to a region of weaker expanding magnetic field, where the beam will form and propagate. The Plasma Physics Laboratory of UnB is designing a Helicon Double Layer Thruster Figure 4.1 - The Helicon Double Layer Thruster Assembly (HDLT) Fig. 4.1. This thruster will employ three types of magnetic coils containing 730, 912 turns with 20 cm internal diameter and a smaller diameter (15 cm) coil with 710 turns of 3 mm diameter copper insulated wire to provide a magnetic axial field within a gradient typically of 200 to 400 Gauss variation along 80 cm in two connected vacuum glass cylindrical chambers with diameter of 10 cm and 15 cm respectively. The vacuum pumping system uses an Edwards two stage mechanical pump working at 5 m3 /h and an Edwards 63 mm diameter Instituto Nacional de Pesquisas Espaciais - INPE 79 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil diffusion pump working with 135 l/s, reaching 10−7 Torr in a system with two connected borosilicate glass vacuum tubes D1 = 15 cm, D2 = 10 cm and total system length L= 100 cm. Plasma generation is made by helicon wave loop antenna positioned over the D2 glass tube at the highest magnetic field region of the system. Using 5 W to 20 W of a RF generator from Amplifier Research Company model 25W1000, with frequency range of 10 to 1000 MHz, it is possible obtain plasmas densities in the 1010 to 1012 part/cm3 with argon gas pressures from 10−3 to 10−4 torr. In this work we will show the design and development of the first brazillian Helicon Double Layer Thruster, the first plasma parameters results together with its plasma diagnostics systems used to perform plasma characteristics measurements such as plasma potential, density and temperature space profiles using emissive and Langmuir probes. Ion energy measurements with gridded retarding potential energy analyser will also be shown. References: Charles C. and Boswell R. Current-free double-layer formation in a high density helicon discharge. Applied Physics Letters vol.82. no.9, march 2003. Instituto Nacional de Pesquisas Espaciais - INPE 80 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P14) ESCAPE PATTERN AND STICKINESS IN A POLOIDALLY DIVERTED TOKAMAK Caroline G. L. Martins[1] , M. Roberto[1] , and I. L. Caldas[2] [1] Departamento de Fı́sica, Instituto Tecnológico de Aeronáutica, São José dos Campos, São Paulo, 12228-900 Brazil. e-mail: [email protected] [2] Universidade de São Paulo, Instituto de Fı́sica 05315-970 São Paulo, SP, Brazil ABSTRACT We analyze a Hamiltonian model that describes magnetic surfaces with rotational number profile similar to those observed in tokamaks with a poloidal divertor. Non-axisymmetric magnetic perturbations are added by external coils used to improve the plasma confinement. To show the influence of magnetic perturbations on the field line escape, we integrate numerically the field line differential equations and obtain the footprints and deposition patterns on the divertor plate. Moreover, we show that the homoclinic tangle describes the deposition patterns in the divertor plate. Additionally, we show that while chaotic lines escape to the divertor plates, some of them are trapped, for many toroidal turns, in complex structures around magnetic islands, embedded in the chaotic region, giving rise to the so called stickiness effect characteristic of chaotic Hamiltonian systems. Instituto Nacional de Pesquisas Espaciais - INPE 81 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P15) DETECTION OF COHERENT STRUCTURES IN SPACE PLASMAS AND ITS RELATION WITH SOLAR WIND TURBULENCE AND MAGNETIC RECONNECTION Pablo R. Muñoz[1] and A. Ojeda González[2,3] [1] Institute of Aeronautical Technology (ITA), São José dos Campos-SP 12228-900, Brazil. e-mail: [email protected] [2] DGE/CEA/National Institute for Space Research - INPE 12227-010 São José dos Campos, SP, Brazil [3] Bolsista do CNPq - Brazil ABSTRACT We implement a method to detect coherent magnetic structures using the Haar discrete wavelet transform (Salem et al., ApJ 702, 537, 2009), and apply it to two different magnetic cloud boundary layer (MCBL) events: (i) an ICME measured by Cluster upstream of the Earth’s bow shock on 2005 January 21 previously studied by Chian and Muñoz (ApJL 733, L34, 2011) and (ii) the turbulent interface between two merging magnetic clouds detected by Wind on 1998 August 20 (see poster P29). The wavelet method is able to detect magnetic coherent structures and extract main features of solar wind intermittent turbulence, such as the power spectral density and the scaling exponent of structure functions. We found observational evidence of magnetically reconnected current sheets in the vicinity of the MCBL for both Cluster and Wind events, where the scaling exponent of structure functions of magnetic fluctuations exhibits multifractal behavior. Using the wavelet technique, we show that the current sheets associated to magnetic reconnection are part of the magnetic coherent structures set responsible for multifractality. By removing them using a filtering criteria, it is possible to recover a self-similar scaling exponent predicted for homogeneous turbulence. Instituto Nacional de Pesquisas Espaciais - INPE 82 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P16) INTERPLANETARY ORIGIN OF GEOMAGNETIC STORMS (PEAK Dst ≤ −50 nT ) DURING THE SOLAR CYCLE 23. E. Echer[1] , W. D. Gonzalez[1] , and B. T. Tsurutani[2] [1] National Institute for Space Research, Sao Jose dos Campos, SP, 12227-010, Brazil. e-mail: [email protected] [2] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, 91109, USA ABSTRACT We have studied the interplanetary origins of moderate (Dst ≤ −50 nT ) and intense (Dst ≤ −100 nT ) geomagnetic storms during the solar cycle 23. Interplanetary parameters and structures that lead to geomagnetic storms were investigated. It was found that all geomagnetic storms were preceded by a southward directed interplanetary magnetic field Bz component (IMF Bs). Thus it was concluded that magnetic reconnection between the IMF Bs and the earth magnetopause field is the main mechanism for solar wind magnetosphere energy coupling during moderate and intense geomagnetic storms. The interplanetary structures that are more important to cause intense storms are magnetic clouds, sheath fields and their combination, while for moderate storms the most important structures are corotating interaction regions and magnetic clouds. However, the distribution of the interplanetary drivers changes with solar cycle phase. The solar wind energy available for magnetic reconnection is estimated and it seems to double from moderate to intense storm and double again from intense to superintese (Dst ≤ −250 nT ) storms. Finally, the overall geomagnetic activity and storm occurrence during the recent deep solar minimum will be compared with previous cycles. Instituto Nacional de Pesquisas Espaciais - INPE 83 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P17) A DOUBLE-CORED FTE FROM BATS-R-US Aline de Lucas[1] , D. Sibeck[2] , W. D. Gonzalez[1] , and M. V. Silveira[1] [1] Instituto Nacional de Pesquisas Espaciais INPE, São Jose dos Campos, São Paulo, Brazil. e-mail: [email protected] [2] NASA Goddard Space Flight Center GSFC, Greenbelt, Maryland, U.S.A. ABSTRACT Flux Transfer Events (FTEs) behave similarly to magnetic portals allowing the energy transfer between the solar wind to the magnetosphere through patchy reconnection. In this work, we show a very interesting case of FTE observed in BATS-R-US output for May 20th 2007 between 21:28 and 21:31 UT. The magnetic signatures show a double-cored FTE. Different plots as well other parameters, in addition to magnetic vector, are analyzed for this event in order to identify its main characteristics. Instituto Nacional de Pesquisas Espaciais - INPE 84 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P18) HILDCAAs AND ASSOCIATED INTERPLANETARY VARIATIONS: SUPERPOSED EPOCH ANALYSES UNDER VARYING SOLAR ACTIVITY AND SEASONAL CONDITIONS Rajkumar Hajra[1] , Ezequiel Echer[1] , Walter D. Gonzalez[1] , and Bruce T. Tsurutani[2] [1]Instituto Nacional de Pesquisas Espaciais (INPE), Sao Jose dos Campos, SP, Brazil. e-mail: [email protected] [2] Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, U.S.A. ABSTRACT We study the solar cycle and seasonal dependences of high-intensity, long-duration, continuous AE activity (HILDCAA) events and associated solar wind/interplanetary variations for ∼ 31/2 solar cycle period, from 1975 through 2011. While 133 events were detected during this period, we studied 99 events when simultaneous interplanetary data were available. The peak occurrence frequencies of the events were noted during the descending phase of the solar cycle. These events had strongest integrated AE intensity, coincident with peak occurrences of high-speed solar wind streams. The event initiation coincided with the slow-to-high speed stream interaction, compressions in solar wind plasma and interplanetary magnetic field (IMF) - typical for corotating interaction region (CIR). The signature of CIR was much prominent for the events occurring during the descending phase and solar minimum, with solar wind speed (Vsw) increases of ∼ 41% and 57% respectively, compared to weak or no CIR structures during the ascending phase and solar maximum. HILDCAAs occurring during different seasons were found to be associated with more or less same interplanetary structures. However, Vsw increases were slightly enhanced during solstices (∼ 40%) than equinoxes (∼ 30%). Spring and fall events were found to occur preferentially in the geoeffective negative and positive IMF sector regions, respectively. Instituto Nacional de Pesquisas Espaciais - INPE 85 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P19) EXTENDED DAYSIDE MAGNETOPAUSE RECONNECTION LINE AS EVIDENCED BY QUASI-SIMULTANEOUS THEMIS OBSERVATIONS Vitor Souza[1,2] , W. D. Gonzalez[1] , D. G. Sibeck[2] , Brian Walsh[2] , D. Koga[1] , and Odim Mendes[1] [1] National Institute for Space Research (INPE), Sao Jose dos Campos, SP, Brazil. e-mail: [email protected] [2] NASA Goddard Space Flight Center, Greenbelt, MD, U.S.A. ABSTRACT In this work we investigate a conjunction of two THEMIS spacecraft (THA and THC) which crossed a reconnecting dayside magnetopause quasi simultaneously. THC sampled the magnetopause boundary at around 14:39 UT on July 07, 2009 slightly duskward (Ygsm = 2.8 Re) and southward (Zgsm = -3.1 Re) of the subsolar point, while only ∼ 5 minutes later THA crossed it at Ygsm = 10.4 Re and Zgsm = -4.8 Re, after skimming the dusk flank magnetopause below the magnetic equator for the past 25 minutes. THEMIS B, located upstream of the Earth’s bow shock, monitored the interplanetary magnetic field (IMF) for this event. The lagged IMF indicated a consistent duskward and southward component for the approximately 1 hour interval which encompassed both the THA and THC magnetopause crossings. The duskward and southward local plasma velocity enhancements sampled by both spacecraft are consistent with a magnetopause crossing southward of a tilted, subsolar x-line as shown by the Gonzalez and Mozer [JGR, 1974] component reconnection model. Further evidence extracted from both 1D and 2D cuts of full 3D ion and electron velocity distributions are presented. These signatures suggest the possibility of a global, extended, long-lasting reconnection line on the magnetopause. Results from a global MHD model for the Earth’s dayside environment at the time of the analyzed event are shown to corroborate this hypothesis. Instituto Nacional de Pesquisas Espaciais - INPE 86 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P20) A REVIEW ON CORONAL HEATING PROBLEM S. S. A. Silva[1] , M. V. Alves[1] , J. C. Santos[2] [1] Instituto Nacional de Pesquisas Espaciais (INPE), Sao Jose dos Campos, SP, Brazil. e-mail: [email protected] [2] Universidade Federal do Paraná, Curtiba, PR, Brazil ABSTRACT One of the most important open questions regarding the sun is how its outer atmosphere, the solar corona, is heated up to millions of kelvin. Nowadays it is believed that the heating question is actually not just a problem addressed to the corona but to the whole solar atmosphere as a coupled system. There are some proposed mechanisms that could create and carry energy required to heat coronal plasma. However, one does not know which mechanism would prevail or exactly how this energy would be dissipated in the highly conducting plasma of the solar corona. This poster presents a brief review on the theory of heating mechanisms for coronal loops in solar active regions as well as the main cooling mechanisms acting on coronal regions. Instituto Nacional de Pesquisas Espaciais - INPE 87 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P21) THE Io PLASMA TORUS Fabiola Pinho Magalhães[1] , W. D. Gonzalez[1] , Mariza P. S. Echer[1] , and Ezequiel Echer [1] [1] Instituto Nacional de Pesquisas Espaciais (INPE), São José dos Campos, SP, Brazil. e-mail: [email protected] ABSTRACT Over the last decades, several spacecrafts have flown past Jupiter’s system. Several in situ measurements gave us important informations about Jupiter’s magnetosphere, Io’s volcanism and the interaction between both. The first evidence of an eletromagnetic connection between Io and Jupiter’s magnetosphere was first evidenced by E. K. Bigg in 1964. Io’s active volcanic plumes expels a considerable amount of material to the atmosphere in the form of ions. A significant fraction of the material scapes as neutral atoms and molecules, principally oxygen and sulfur atoms. These neutrals accompany Io in its orbits about Jupiter until they are ionized through electron impact and charge exchange. Once ionized, the ions are accelerated to the nearly corotational flow of the ambient plasma, forming a torus of ions surrounding Jupiter, the Io plasma torus. The Io plasma torus is a donut-shaped ring, mainly composed by oxygen and sulfur atoms and their compounds. The torus is about 2 Jupiter radii in width and is centered on Io’s orbit around Jupiter at a distance of 5.9 Rj. In this work we’ll be presenting the main characteristics of the Io plasma torus, composition and the groundbased observation from [SII] 6731 angstrom. Instituto Nacional de Pesquisas Espaciais - INPE 88 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P22) GLOBAL MUON DETECTOR NETWORK - COSMIC RAYS AS OTHER POINT OF VIEW FOR SPACE WEATHER’S APPLICATIONS Rockenbach, M.[1] , Dal Lago, A.[2] , Schuch, N.J.[1] , Munakata, K.[4] , Kuwabara, T.[6] , Oliveira, A.G.[3] , E. Echer[2] , Braga, C.R.[2] , Mendonça, R.R.S.[2] , Kato C.[4] , Yasue, S.[4] , Tokumaru, M.[5] , Bieber, J.W.[6] , Evenson P.[6] , Duldig, M. L.[7] , Humble, J. E.[7] , Al Jassar, H. K.[8] , Sharma M. M.[8] , Sabbah, I.[9,10] [1] Southern Regional Space Research Center - CRS/INPE-MCTI - P.O. Box 5021, 97110-970 - Santa Maria, RS - Brazil. e-mail: e-mail: [email protected] [2] National Institute for Space Research (INPE), 12227- São José dos Campos, Brazil [3] Instituto de Pesquisa e Desenvolvimento, Universidade do Vale do Paraı́ba, São José dos Campos, Brazil [4] Physics Department, Shinshu University, Matsumoto, Nagano 390-8621, Japan [5] Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan [6] Bartol Research Institute and Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, U.S.A. [7] School of Physical Sciences, University of Tasmania, Hobart, Tasmania 7001, Australia [8] Physics Department, Faculty of Science, Kuwait University, Kuwait city, Kuwait [9] Department of Natural Sciences, College of Health Sciences, Public Authority of Applied Education and Training, Kuwait City, Kuwait [10] Astronomy Department, Faculty of Science, King Abdulaziz University, Jeddah, Saudi Arabia ABSTRACT In this work, we summarize the development and current status of the Global Muon Detector Network (GMDN). The GMDN started in 1992 with only two muon detectors. It has consisted of four detectors since the Kuwait muon hodoscope detector was installed in March 2006. The present network has a total of 60 directional channels with an improved coverage of the sunward Interplanetary Magnetic Field (IMF) orientation, making it possible to continuously monitor cosmic ray precursors of geomagnetic storms. The data analysis methods developed also permit precise calculation of the three dimensional cosmic ray anisotropy and gradient Instituto Nacional de Pesquisas Espaciais - INPE 89 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil on an hourly basis free from the atmospheric temperature effect and analysis of the cosmic ray precursors free from the diurnal anisotropy of the cosmic ray intensity. The main results will be presented. Instituto Nacional de Pesquisas Espaciais - INPE 90 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P23) A COMPARATIVE STUDY OF LAGRANGIAN TECHNIQUES FOR DETECTING COHERENT STRUCTURES IN THE SOLAR PHOTOSPHERE Jenny M. Rodrı́guez[1] , Abraham C.-L. Chian[1,2] , and Erico L. Rempel[1,3] [1] National Institute for Space Research (INPE), São José dos Campos-SP 12227010, Brazil. e-mail: [email protected] [2] Observatoire de Paris, LESIA, CNRS, 92195 Meudon, France [3] Institute of Aeronautical Technology (ITA), São José dos Campos-SP 12228-900, Brazil ABSTRACT The Lagrangian technique is used to study individual fluid elements and how the dynamics of individual particles along the flow paths can be used to detect coherent structures responsible for transport barriers in fluids in general. In this poster concepts of Lagrangian Coherent Structures (LCS), Finite time Lyapunov Exponent (FTLE), the Probability Density functions (PDFs) will be reviewed and applied to observed data in the solar photosphere and numerical simulations of convection in magnetized fluid in a plane layer. Instituto Nacional de Pesquisas Espaciais - INPE 91 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P24) COMPARATIVE STUDY OF THE MAGNETIC AND PLASMA PRESSURE FORCES IN THE MAGNETOSHEATH Germán Fariñas Pérez[1] , W. D. Gonzalez[1] , Flavia R. Cardoso[2] , and Ramon E. Lopez[3] [1] National Institute for Space Research- INPE, SJC, SP, Brazil. e-mail: [email protected] [2] Escola de Engenharia de Lorena/Universidade de São Paulo- EEL/USP, Brazil [3] Dept. of Physics, University of Texas at Arlington, Arlington, Texas, USA ABSTRACT Under normal circumstances, when the amplitude of the interplanetary magnetic field (IMF) is small, the dominant force in the magnetosheath is given by the plasma pressure gradient. In this situation the portion of the ionospheric potential generated by the magnetic reconnection process have a linear behavior in terms of the interplanetary electric field. In the other ~ may become the dominant force in regime, when the IMF is large, the magnetic force J~ × B the magnetosheath and can affect the dynamics of the solar wind flux transport through the magnetosheath saturating the ionospheric potential. We use the BATS-R-US global magnetohydrodynamic (MHD) simulation code to measure the forces acting on the magnetosheath under purely southward IMF and constant solar wind conditions. A comparison between the magnitudes of the pressure gradient and magnetic forces is presented for small and large ~ values of southward IMF (Bz ). A qualitative study of the role of the magnetic force J~ × B on the behavior of the solar wind geoeffective length is carried out for different values of Bz . Instituto Nacional de Pesquisas Espaciais - INPE 92 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P25) VALIDATION OF THE RECONNECTION COMPONENT MODEL AND DETERMINATION OF THE RECONNECTION X-LINE FOR DIFFERENT CONFIGURATIONS OF THE INTERPLANETARY MAGNETIC FIELD USING THE 3D MHD BATS-R-US MODEL Paulo Ricardo Jauer[1] , W. D. Gonzalez[1] , and Cristiane Loeschen[1] [1]Instituto Nacional de Pesquisas Espaciais-INPE, Brasil. e-mail: [email protected] ABSTRACT When the solar wind and the geomagnetic field interact at the magnetopause, the IMF connects to the geomagnetic field along a line known as reconnection X-line. As a result, the interplanetary electric field is mapped to inner regions of the magnetosphere, playing a key role in the dynamics of the magnetosphere. In order to estimate these fundamental physical processes Gonzalez and Mozer (1974) developed a simplified quantitative three-dimensional model of reconnection at the magnetopause. The objective was to determine the electric potential due to reconnection for an arbitrary orientation of the IMF. This model is known as the reconnection component model. Our goal is to make use of the 3D model MHD BATS-RUS, to test the component reconnection model and its validation, modeled for a set of several IMF orientations. Where the reconnection angle is small, reconnection due the component model is not expected at the subsolar region, but the complementary “parallel” reconnection model may occur at high latitudes. Instituto Nacional de Pesquisas Espaciais - INPE 93 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P26) HALL ELECTRIC FIELD IN ASYMMETRIC MAGNETIC RECONNECTION D. Koga[1] , W. D. Gonzalez[1] , F. S. Mozer[2] , and F. R. Cardoso[3] [1] National Institute for Space Research (INPE), São José dos Campos, SP, Brazil. e-mail: [email protected] [2] Space Sciences Laboratory, University of California, Berkeley, CA, USA [3] School of Engineering (EEL), University of São Paulo, Lorena, SP, Brazil ABSTRACT Magnetic reconnection would take place in an asymmetric geometry at the earth’s magnetopause. We analyze 12 magnetic reconnection events observed by the POLAR satellite. These events show a clear existence of the unipolar Hall electric field variation during the magnetopause crossings. The Hall electric field will be compared with the guide field, plasma density, Alfvén speed, and reconnection rate in order to show the importance to reconnection processes. Furthermore, the existence of the so-called “Larmor electric field” (Malakit et al. 2013) will be discussed using the POLAR and the THEMIS data. Instituto Nacional de Pesquisas Espaciais - INPE 94 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P27) OBSERVATION OF FUNDAMENTAL MAGNETOPAUSE RECONNECTION PARAMETERS BY THE POLAR SATELLITE Walter D. Gonzalez[1] , Daiki Koga[1] , Barbara Ribeiro[2] , Forrest Mozer[3] , Paul Cassak[4] , and Jack Scudder[5] [1] Geophysics Division/CEA - INPE , Sao Jose dos Campos , SP, Brazil. e-mail: [email protected] [2] Physics Department, USP - São Paulo, Brazil [3] Space Sciences Lab - University of California, Berkeley, USA [4] Physics Department - West Virginia University, USA [5] Physics and Astronomy Department - University of Iowa, USA ABSTRACT For some well defined passes at the diffusion region of magnetopause reconnection by the POLAR satellite we have estimated the reconnection rate as defined by the normal component of the magnetopause magnetic field divided by the reconnecting component of the magnetosheath magnetic field. From this we have obtained values for the reconnection electric field and for the speed of reconnection. The diffusion regions of the studied events correspond well to the reconnection x-line expected from the Gonzalez-Mozer (1974) reconnection model and the plasma beta values are also in accord with the reconnection criteria of Swisdak et al (2003) as a function of the corresponding reconnection clock angles. It is also seen that the varying plasma beta and reconnection rate values during the magnetopause crossings are strongly anticorrelated. This may imply that magnetosheath plasmas with different plasma beta values (such as those found in magnetic clouds and in high speed streams) lead into a higher or lower efficiency in magnetopause reconnection, with a consequent higher or lower efficiency in the transfer of energy and momentum from the solar wind to the magnetosphere. Instituto Nacional de Pesquisas Espaciais - INPE 95 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P28) MAGNETIC FIELD AND FLOW VARIATIONS ASSOCIATED WITH A TRANSIENT EVENT OBSERVED AT THE MAGNETOPAUSE BY THE THEMIS SPACECRAFT M. V. D. Silveira[1] , D. G. Sibeck[2] , W. D. Gonzalez[1] , and D. Koga[1] [1] National Institute for Space Research (INPE), São José dos Campos, SP, Brazil. e-mail: [email protected] [2] NASA Goddard Space Flight Center, Greenbelt, MD, USA ABSTRACT Flux transfer events generated at the Earth’s magnetopause would play a crucial role for magnetospheric and ionospheric dynamics because they are a portal of the solar wind mass flux, energy and momentum into the magnetosphere. The fact that THEMIS mission consists of 5 satellites will be enable us to study FTEs structures in detail. During the interval from 22:32 UT to 22:36 UT on June 10, 2007, four of the five THEMIS spacecraft recorded clear bipolar FTE variations in the magnetic field component normal to the nominal magnetopause. The perturbation was associated with other variations in the magnetic field and plasma parameters, including a high ion flow speed immediately behind and ahead of the structure and a distinct flow variation inside the structure. THEMIS B, located deepest inside the magnetosphere, observed plasma perturbations but no significant magnetic field variation. Consequently the extent of the plasma perturbations exceeded that of the magnetic field perturbations. We can interpret the observations as evidence for a flux rope-like structure moving faster than the ambient plasma. Instituto Nacional de Pesquisas Espaciais - INPE 96 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P29) CHARACTERIZATION OF A DOUBLE FLUX-ROPE MAGNETIC CLOUD OBSERVED BY ACE SPACECRAFT ON AUGUST 19-21, 1998 A. Ojeda González[1,4] , W. D. Gonzalez[1] , O. Mendes[1] , M. O. Domingues[2] , and P. R. Muñoz[3] [1] DGE/CEA/National Institute for Space Research - INPE 12227-010 São José dos Campos, SP, Brazil. e-mail: [email protected] [2] LAC/CTE/National Institute for Space Research - INPE 12227-010 São José dos Campos, SP, Brazil [3] Institute of Aeronautical Technology (ITA), Sao Jose dos Campos-SP 12228-900, Brazil [4] Bolsista do CNPq - Brazil ABSTRACT Several researchers have studied magnetic cloud (MC) cases of double flux rope configuration with apparent asymmetry. A Grad-Shafranov reconstruction technique allows the derivation of the local magnetic structure from data of a single spacecraft. In this work, we examine the event that occurred in Aug. 19-21, 1998 using solar wind measurements collected by ACE. The results obtained show two cylindrical flux ropes next to each other, where a single X point forms between them. In all possible combinations of two bipolar MCs, the magnetic field lines between them are antiparallel in eight cases: SWN-SWN, SWN-SEN, SEN-SWN, SENSEN, NWS-NWS, NWS-NES, NES-NWS, NES-NWS. If clouds are under magnetic coupling, reconnection evidences are expected from the interaction between them. The cross-section between two bipolar clouds (SEN-SWN) is shown. In the opposite corners of the X point, the magnetic fields are antiparallel. The spacecraft crosses an X point and observes plasma jets within a bifurcated current sheet in the solar wind (see poster P15), and provides further direct evidence that such jets result from reconnection. The residual velocity in the deHoffmannTeller frame at ACE is perpendicular to the magnetic field line in the reconnection region. In principle, it is possible to adjust a two-dimensional model considering the most common separator reconnection, in which four separate magnetic domain exchange magnetic field lines. The magnetic configuration reconstructed confirms the initial hypothesis, i.e., the existence of two bipolar MCs (SEN-SWN) with reconnection between them. Acknowledgments Acknowledgments to Christian Möstl and Charles J. Farrugia, authors of Matlab code for Grad-Shafranov reconstruction of magnetic flux ropes. Instituto Nacional de Pesquisas Espaciais - INPE 97 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P30) 3D HALL MHD GLOBAL SIMULATION OF THE MAGNETOPAUSE RESPONSE TO THE APRIL, 2010 EVENT: ANALYSIS OF POSSIBLE MAGNETIC RECONNECTION REGIONS C. Loesch[1] , M. V. Alves[1] , P. R. Jauer[1] , and W. D. Gonzalez[1] [1] National Institute for Space Research (INPE), Brazil. e-mail: [email protected] ABSTRACT On 05 April 2010, the arrival of a CME-driven shock and its turbulent sheath at 1AU were observed by both ACE and Wind satellites with an interplanetary magnetic field (IMF) that turned southward to an average of -15 nT. Such arrival was followed by the first significant geomagnetic storm of solar cycle 24, with a minimum Dst of -72 nT. In this work we present a time-dependent hall magnetohydrodynamic (MHD) simulation of the Earth’s magnetopause response during the geomagnetic storm. Our simulations were performed with the Space Weather Modeling Framework, a tri-dimensional MHD global model. We have consider a greater grid refinement at the dayside magnetopause near the subsolar region in order to analyze possible magnetic reconnection regions at the dayside magnetopause. The search for dayside reconnection initiates at the time the Bz component of the magnetic field turns southward and ends when it turns northward (at the first day of the geomagnetic storm). We estimate the inclination of the reconnection line at the dayside magnetopause using the model presented by Gonzalez and Mozer (1974). We also discuss the influence of the xcomponent of the IMF on the location of the reconnection region. Our results are compared to the 4-line junction concept discussed by Laitinen et. al (2006), who suggested that the reconnection separator line can be identified as the region where the magnetic field lines of different topological properties meet. Our comparison presents an agreement within the methods and our results indicate the possibility of simultaneous subsolar and high latitude reconnection regions as the simulation evolves. Instituto Nacional de Pesquisas Espaciais - INPE 98 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P31) MULTI-WAVELENGTH OBSERVATION AND ANALYSIS OF A COHERENT, WAVE-LIKE PROPAGATING INTENSITY DISTURBANCES ALONG PSEUDO-OPEN FIELD LINES ABOVE A SUNSPOT Tardelli Stekel[1] , Guillermo Stenborg[2] , and Alisson Dal Lago[1] [1] National Institute for Space Research, São José dos Campos, SP, Brazil. e-mail: [email protected] [2] George Mason University, Fairfax, Virginia, USA ABSTRACT The observation of fast and slow magnetoacoustic waves were only possible through highresolution extreme ultraviolet (EUV) images, such as those provided by imagers onboard the SOHO, TRACE, STEREO, and SDO missions. These observations created the observational foundation for new methodologies for coronal plasma diagnostics, i.e., coronal seismology. We have developed a technique to create height-time intensity maps along arbitrary paths on EUV images from different instruments (e.g., STEREO/EUVI and SDO/AIA) in all available channels simultaneously. In this work, we report the first direct observation (along with a comprehensive kinematical characterization) of an arc-shaped wave-like front recorded in several SDO/AIA channels on 2011 July 6. The front is observed to propagate coherently along several pseudo-open field lines with origin on a sunspot AR 1243. Wavelet-processed SDO/AIA images make the wave-like disturbances clearly discernible with the naked eye. The intensity disturbances propagate with an average plane-of-sky phase velocity of about 50 km/sec in the 131 Å, 171 Å, 193 Å, 211 Å, 304 Å and 335 Å channels, exhibiting a ∼ 3 min periodicity in all cases. Its origin could be tracked down to a higher-than-average intensity point inside the umbra of the corresponding spot (i.e., an umbral dot) as observed in the 1600 Å and 1700 Å SDO/AIA channels. The intensity of the source oscillates in phase with the wave-like phenomenon observed in the other channels. Instituto Nacional de Pesquisas Espaciais - INPE 99 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P32) MAGNETIC CONFIGURATION OF A FLARING ACTIVE REGION L. Balmaceda[1] , J. Palacios[2] , L. E. Vieira[1] , and A. Dal Lago[1] [1] National Institute for Space Research, São José dos Campos, SP, Brazil. e-mail: [email protected] [2] Universidad de Alcalá, Spain ABSTRACT Solar flares are one of the most extreme phenomena in the atmosphere of the Sun, releasing huge quantities of energy in very short time scales. High resolution magnetic field data represent an invaluable tool to investigate the conditions and the changes in the regions where such phenomena take place. Here, we study the temporal and spatial evolution of the active region 11429 (N17E15) associated to an intense flaring activity observed during 2012 March 6 to 9. In particular, we study the evolution of the photospheric magnetic field in this active region, and the changes from the original configuration. For this, we use a time series of vector field maps with high spatial resolution obtained with Hinode/SP instrument. We estimate the total shear and the weighted mean shear in order to analyze the departure from potentiality before and after a flare occurrence as a possible triggering mechanism. Instituto Nacional de Pesquisas Espaciais - INPE 100 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P33) THE GEOMAGNETIC RESPONSE TO EXTREME SOLAR WIND EVENTS A. Dal Lago[1] , E. Echer[1] , L. A. Balmaceda[1] , R. Rawat[1] , L. E. A. Vieira[1] , T. R. C. Stekel[1] , and W. D. Gonzalez[1] [1] National Institute for Space Research, São José dos Campos, SP, Brazil. e-mail: [email protected] ABSTRACT Coronal mass ejections observed in the interplanetary space (ICMEs) are found to be one of the most frequent sources of out-of-the-ecliptic interplanetary magnetic fields. Geomagnetic storms are related to these fields when they possess a southward pointing component. ICME internal fields and sheath fields associated with their interplanetary shocks were found to be the dominant origins of Intense (Dst <100 nT) and very intense (Dst<-200 nT) geomagnetic storms in the ascending phase and maximum of the solar cycle 23. Extreme events, in which Dst<-400 nT, are less frequent, but they are all associated to ICMEs. Recent studies show that these events occur nearly once every 11 year solar cycle. We investigate the geomagnetic response to these extreme solar wind conditions using observations and modeling. Instituto Nacional de Pesquisas Espaciais - INPE 101 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P34) MODELING THE EQUATORIAL AND LOW LATITUDE IONOSPHERE RESPONSE TO AN INTENSE X-CLASS SOLAR FLARE P. A. B. Nogueira[1] , J. R. Souza[1] , M. A. Abdu[1] , R. Paes[1] , J. Sousasantos[1] , M.S. Marques[1] , R.Y.C. Cueva[1,2] , C.M. Denardini[1] , I.S. Batista[1] , H. Takahashi[1] , and S.S. Chen[1] [1] Divisão de Aeronomia, Instituto Nacional de Pesquisas Espaciais, São José dos Campos, 12227-010, São Paulo, Brazil. e-mail: [email protected]; [email protected] [2] Centro de Radio Astronomia e Astrofı́sica Mackenzie, CRAAM, Presbyterian Mackenzie University, São Paulo, Brazil ABSTRACT We have investigated the ionospheric response close to the subsolar point due to the strong solar flare (X2.8) that occurred on May 13th , 2013. The present work discusses the sudden disturbances observed in the major ionospheric parameters, such as in the E-region current system as obtained from ground based magnetometer observations near magnetic equator, and at low-latitude and mid-latitude stations. A strong intensification of the eastward Equatorial Electrojet (EEJ) was observed over Peru. The dayside ionosphere showed an abrupt increase of the Total Electron Content (TEC) over South America, especially over the low latitude region, due to the flare enhanced ionizing solar radiation flux. In this work we have used the Sheffield University Plasmasphere-ionosphere Model (SUPIM) to model the TEC enhancement as arising from the flare enhanced solar EUV flux soft X-rays. The model results are compared with the observational data on the TEC and solar EUV and X-ray fluxes. Instituto Nacional de Pesquisas Espaciais - INPE 102 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P35) STORM ELECTRIC FIELD EFFECTS IN THE LOW-LATITUDE IONOSPHERE J. R. Souza[1] , B. G. Fejer[2] , M. A. Abdu[1] , I. S. Batista[1] , and G. J. Bailey[3] [1] Instituto Nacional de Pesquisas Espaciais, Caixa Postal 515, São José dos Campos, SP, Brasil. e-mail: [email protected] [2] Center for Atmospheric and Space Science, Utah State University, Logan, UT, USA [3] Department of Applied mathematics, University of Sheffield, Sheffield, S3 7RH, U.K ABSTRACT Geomagnetic storms often cause large spatial and temporal perturbations in the equatorial and low latitude plasma densities. Ionospheric ground based observations have been made in the Brazilian equatorial and low latitude region during several geomagnetically disturbed periods. We use Sheffield University Plasmasphere Ionosphere Model (SUPIM) and extensive ionospheric measurements over Brazil and Peru to study in detailed the temporal, latitudinal and longitudinal distribution of the ionospheric plasma densities during large geomagnetic storms. SUPIM is a theoretical model in which coupled time-dependent equations of the continuity, momentum and energy balance are solved along closed magnetic field lines to give values for the densities, temperatures and field-aligned fluxes of the electrons and of several ions. Electric fields derived from ionospheric measurements are used as input parameter for the model calculations. We will focus mostly on the global time-dependent response of the Appleton anomaly to large changes in the equatorial zonal electric fields during the early phases of large geomagnetic storms. Instituto Nacional de Pesquisas Espaciais - INPE 103 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P36) SIMULATION OF IDEAL MHD MODEL IN THE CONTEXT OF ADAPTIVE MULTIRESOLUTION USING THE HYPERBOLIC DIVERGENCE CLEANING APPROACH Anna Karina F. Gomes[1] , Margarete O. Domingues[2] , Odim Mendes[3] , Kai Schneider[4] [1] Pós-graduação em Computação Aplicada, Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, Brasil. e-mail: [email protected] [2] Laboratorio Associado de Computaçlão e Matemática Aplicada, Instituto Nacional de Pesquisas Espaciais, São José dos Campos, São Paulo, Brasil [3] Divisão de Geofı́sica Espacial, Instituto Nacional de Pesquisas Espaciais, Sao José dos Campos, São Paulo, Brasil [4] M2P2-CNRS & Centre de Mathematiques et D’Informatique (CMI), AixMarseille Université, 38 rue F. Joliot-Curie, 13451 Marseille Cedex 20, France ABSTRACT In this work, we present a new approach to the numerical simulation of a conservative twodimentional ideal magnetohydrodynamics model: an adaptive multiresolution method. This multiresolution method is based on Ami Harten’s cell average multiresolution approach, which permits a locally refined spatial grid while controlling the error. The main goal of this work is evaluate the numerical stability and the effectiveness of the multiresolution algorithm for the current system of differential equations. In the numerical context, the divergence of magnetic field does not remain zero. Thus, we use the Generalized Lagrangian Multiplier (GLM) approach with a mixed hyperbolic-parabolic correction to control the magnetic field constraint, by avoiding non-physical behavior and dispersion of the numerical solution. To simulate the MHD model, we choose the finite volume method discretization, which is very suitable for conservation laws. To show the efficiency of the multiresolution approach when compared with the non-adaptive one, we present the simulation of MHD classical problems and the CPU time and memory savings obtained. The accuracy of the adaptive computations is measured by comparing it with a reference solution computed on a fine regular grid. Instituto Nacional de Pesquisas Espaciais - INPE 104 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil P37) DEGRADATION OF THE MAGNETIC STRUCTURE OF ELONGATED ICMES BY INTERIOR RECONNECTION Raymond L. Fermo[1] , M. Opher[2] , J. F. Drake[3] [1] Astronomy Department, Boston University, Boston, MA, USA. e-mail: [email protected] [2] Astronomy Department, Boston University, USA [3] Maryland University, USA ABSTRACT The magnetic structure of interplanetary coronal mass ejections (ICMEs) is often considered to be a magnetic cloud, characterized by a smooth rotation of the magnetic field. However, perhaps as few as 30% of observed ICMEs display such a coherent helical flux rope geometry (Gosling et al., 1990). We propose that reconnection in the interior of the ICME could result in a complex stochastic magnetic field and the destruction of the magnetic cloud structure. Such reconnection events within the core of ICMEs have been seen in recent in situ observations (Gosling et al., 2007). We show that reconnection can be initiated as the ICME flux rope becomes elongated in the latitudinal direction as it propagates through the interplanetary medium. This elongation forces the ICME flux rope from its force-free Taylor state, and as a consequence, the flux rope will attempt to relax back to that minimum energy state. Subject to the constraints that the toroidal flux and magnetic helicity are invariant, this relaxation must be mediated by reconnection of the interior magnetic field. We present MHD simulations of an elongated flux rope which has evolved away from the Taylor state and show that reconnection at many surfaces produces a stochastic magnetic field as the system evolves back to a minimum energy state configuration. Instituto Nacional de Pesquisas Espaciais - INPE 105 5 DISCUSSION Question I: Usually the topology of reconnection is drawn with well behaved approaching magnetic fluxes (X direction) and also well behaved exiting fluxes (Z direction) at distances sufficiently far from the diffusion region (with the current sheet pointing in the Y direction). In the diffusion region the reconnecting fluxes go into complex micro processes that allow them to “get cut” and later to “reconnect” and exit. How do the magnetic fluxes “get cut” and “reconnect”, transforming themselves into a turbulent regime and then getting back to a well behaved topology again? What are the main physical processes responsible for those topological changes? Replies by Prof. Scudder: Maxwell’s equations are about fields, not field lines-although the latter has a utility in some cases for explaining how fields behave. The “cutting” and “reconnection” short hands are after the effect descriptions, not explanations of how this happens. Maxwell’s equations are about the 4-vector potential and that description is smooth in space and time. In the short scaled “diffusion” region it is not longer possible to prove that their is a well defined evolutionary equations for “field lines”. If one remains in the dialect of describing the behavior of magnetic field lines this lapse of an equation of motion for them requires a discontinuity in their causal description, that clever popularizers have dubbed cutting and reconnection. From this vantage point the question “how do they get cut and reconnect” is not a question that theory at that level will ever clarify. If one agrees to go to the 4 vector potentials of Maxwell one does obtain an evolutionary description in space and time that is smooth. While B(x, y, z, t) as curl of A(x, y, z, t) at any given time has a definite field line topology, that topology is not predictive of the topology of B(x, y, z, t + dt). The MHD regimes does not require the 4-vector potential to predict the rearrangement of field lines; at some level the ubiquitous simplifications that MHD can afford, does not serve the student well to predict what can happen when the foundations of MHD are supplanted in strong gradient current channels. It is widely subscribed that the non-ideal corrections to the generalized Ohm’s law that preclude field and/or flux preservation under the evolution equations is 106 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil generally dominated by the agyrotropic electron pressure tensor, with possible corrections from inertial terms. More generally this regime is indicated as sites where the curl of the non-ideal electric field cE + U e × B not equal zero. An agyrotropic electron pressure tensor generally fulfills this type of violation and microphysically corresponds to the disruption of the magnetization of the bulk of the plasma electrons. Colloquially this implies that the approximations of guiding center theory for electrons are disrupted in these narrow current channels. The most commonly cited approximation involved in guiding center theory is the gyroradius over scale of variation is small. Since Vasyliunas (1975) and the most recent full PIC codes of the process agree that this and other underpinnings of guiding center theory for electrons is disrupted in the electron diffusion region. Prof. Priest: In 2D the way that field lines enter a diffusion region, slip through the plasma and break at the X-point is well understood in resistive MHD, as described by a magnetic flux velocity. In 3D the process is completely different, since the field lines continuously change their connections as they are passing through the diffusion region, and it is not possible to define a single flux velocity. Instead the field lines flip as the magnetic helicity changes and you need a new notion of a dual flux velocity, one based on the field lines whose ends are entering the diffusion region and the other on those that leave. Dr. Zenitani: In order to discuss these topological issues, one has to define the motion of the magnetic field line, but this is notoriously difficult in a non-ideal plasma. Mathematically, the field-line motion and the plasma flow are different, and the reconnection process can be defined when there is no topology conserving velocity. Physically, the plasmas (electrons) slip from the ideal E × B flow in an average sense, consume the magnetic energy, and then diverge into bidirectional outflows. I am still trying to intuitively understand the connection between these two aspects. Prof. Eyink: It is a mythological belief that magnetic flux lines can be interpreted to “move” in a well-behaved manner in a high conductivity plasma. It is also a myth that reconnecInstituto Nacional de Pesquisas Espaciais - INPE 107 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil tion occurs only in isolated “diffusion regions”. Both myths are false in almost any astrophysical plasma, because of prevalent MHD turbulence. Proofs of flux-freezing for ideal MHD in standard textbooks (e.g. Chandrasekhar, 1961) implicitly assume smooth, laminar flow and the theorem statements are false for turbulent flow, even at infinite conductivity. In the presence of MHD turbulence, magnetic field lines can be interpreted to “move” and magnetic flux is conserved only in a novel & surprising stochastic sense. Motion of field lines becomes as indeterministic as motion of quantum particles! Reconnection in the sense of breakdown of standard flux-preservation –the Greene definition –occurs everywhere in MHD turbulence, not only at the most intense current sheets. Standard flux-freezing emerges as an approximate property, when the turbulent fluctuations of plasma velocity & magnetic field are small compared with the large-scale magnetic fields and flow velocities. The notion of “cutting” of field lines is also misleading. There is often topological change of large-scale magnetic flux structures, but it doesn’t occur by “cutting” (which presumes regular prior motion). Reconnection is better understood as “relative diffusion” of ionized plasma and magnetic field lines. The “frozen-in property” of magnetic lines means that two charged particles which start on a single magnetic field line share a single field line for all time (Newcomb, 1958). This property is everywhere violated in MHD turbulence, and plasma diffuses readily across field lines. This leads to topology change of large-scale magnetic flux structures but without any discontinuous process of “cutting” of individual lines. As a matter of fact, small-scale MHD turbulence has itself extremely complex and every-changing magnetic topology, with complex tangles of neighboring field lines explosively (super-chaotically) separating in space by turbulent wandering (Lazarian & Vishniac,1999). The physical process involved in the relative diffusion of plasma and magnetic fields is microscopically tiny non-ideal electric fields (from various possible sources, such as plasma resistivity, pressure tensor, electron inertia, etc). However, the diffusion effect of these tiny electric fields is vastly magnified by turbulent relative dispersion (Richardson dispersion). It is possible in principle to take the mathematical limit where the non-ideal electric fields vanish completely and reconnection will still occur! Thus, to calculate reconnection rates, topological outcomes, etc. It suffices to use an MHD description, whenever there is a long range of MHD turbulence (the solar wind, solar flares, solar chromosphere, CMES, accretion disks, but not the Earth’s magnetosphere!) Instituto Nacional de Pesquisas Espaciais - INPE 108 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil Question II: A fairly large body of literature exists about studies on magnetic field reconnection (based on theories, observations and computer simulations), which describe the internal region of reconnection (diffusion region) and the external regions most of the times separately, with a large gap of understanding about the interdependence between both regions. Among basic issues related with this problem, one does not know how the external plasmas act in the definition of the reconnection rate, which is mostly defined locally at the diffusion region and at times with the external region only providing some very general boundary conditions to that definition. In particular, for magnetopause reconnection, it would be important to understand the global coupling of physical processes involving the dynamics of the Bow shock, the magnetosheath, the magnetosphere and the reconnection process at the magnetopause. Although such a global study is certainly complex, how can at least an overall “flow chart” description be obtained? Replies by Prof. Scudder: This situation is common in boundary layer physics. The EDR is a boundary layer that affords a connection between external regions that are increasingly more ideal insofar as MHD approximations are concerned. This problem between LOCAL MHD boundary conditions on the inflow and exhaust, is only compounded by the contextual system boundary conditions mentioned in the question. These considerations are gradually coming into focus; among the issues are the role of transient local MHD boundary conditions caused by the turbulence of the shock and foreshock layers impinging on the sheath side of the current layer. At present the flow chart would include a list of mechanisms that are capable of (i) changing the time independent assumption of the local MHD boundary conditions usually assumed, or (ii) changing the spatial uniformity of the the local MHD boundary conditions, such as having undulations in properties that are significant across the 10-100 ion gyroradii scales currently assumed to be planar in the present modeling. Clearly the physics of these layers becomes more complicated with Kelvin-Helmholtz waves traveling along the current channel for example. To explore Instituto Nacional de Pesquisas Espaciais - INPE 109 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil these effects requires global modeling of the magnetopause current channel together with the shock, foreshock, and realistic magnetosphere. This type of modeling is just coming of age. Prof. Priest: Most studies of reconnection do indeed treat both the external region and the diffusion region and the relation between them. In 2D steady state resistive reconnection this is now well understood. The rate of reconnection is defined as the rate at which magnetic field lines are brought in towards the reconnection region. This rate depends on the details of the inflow profile, on whether the reconnection is driven or is spontaneous and on whether the resistivity is enhanced or not in the diffusion region. Dr. Zenitani: I do not fully get this question. Given that this asks a general way to discuss the (local) reconnection properties in a global topology, I think it is still difficult to discuss this issue due to the limited computer resource and the complexity of the data. However, we could learn from recent evolution of MHD reconnection. The plasmoid-mediated reconnection may be understood as small local Sweet-Parker reconnections in a global current sheet. Prof. Eyink: Based on the previous answer, the division into an “external region” and an “internal region” is misleading in the presence of MHD turbulence. However, large-scale, high-strength magnetic flux structures which are diffusing only slowly in background turbulence may long persist. When such large-scale structures with an oppositelydirected magnetic field component (as well as possibly a shared component, or guide field) happen to collide, then the turbulent diffusion allows the stored magnetic energy to be rapidly released. The turbulent zone between the structures is the analogue of a “diffusion region” or “current sheet”, but this zone may be many orders of magnitude wider than the proton gyroradius or proton skin depth (up to 6 orders of magnitude larger in the the solar wind (Gosling et al., 2006) and in post-CME current sheets (Susino et al., 2013)). If the background turbulence level is too low to yield rapid reconnection, other mechanisms (e.g. 3D “plasmoid instability” in the MHD regime or plasma physics for smaller structures) may lead to initial reconnection, which generates turbulence in the “internal region” and leads to faster Instituto Nacional de Pesquisas Espaciais - INPE 110 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil reconnection. The rate of reconnection is thus not “mostly defined locally” but depends on a complex of factors, including the initial laminar or turbulent state of the plasma. In fact, to explain solar flares one must avoid fast reconnection to allow a charging phase where magnetic energy slowly builds up. Instituto Nacional de Pesquisas Espaciais - INPE 111 6 LIST OF PARTICIPANTS No. NAME 1 Eugene N. Parker 2 Maha A. Abdalla 3 4 5 6 7 Amitava Bhattacharjee Jörg Büchner Paul Cassak William Daughton A. M. Du 8 9 10 11 Gregory L. Eyink Terry Forbes Stephen A. Fuselier Klaus Galsgaard 12 Daniel Gomez 13 Gerhard Haerendel 14 15 16 17 Gunnar Hornig Hugh Hudson Homayoun Karimabadi Robert Ergun 18 19 20 Alex Lazarian Ramon Lopez Forrest S. Mozer 21 Rumi Nakamura 22 23 24 25 Merav Opher Anatoli Petrukovich E. R. Priest Philip Pritchett INSTITUTION University of Chicago IGPP, University of California, Los Angeles Princeton University Max Planck Institute West Virginia University Los Alamos National Laboratory Geophysical Institute, Chinese Academy of Sciences, Beijing Johns Hopkins University University of New Hampshire Southwest Research Institute Niels Bohr Institute, University of Copenhagen IAFE, Universidad de Buenos Aires Max Planck Institute for Extraterrestrial Physics, Garching University of Dundee University of California, Berkeley UCSD LASP University of Colorado, Boulder, CO University of Wisconsin, Madison University of Texas, Arlington Space Science Laboratory, University of California, Berkeley Space Research Institute, Austrian Academy of Science Boston University IKI St. Andrews University University of California, Los Angeles 112 COUNTRY USA USA USA Germany USA USA China USA USA USA Dennmark Argentina Germany UK USA USA USA USA USA USA Austria USA Russia UK USA Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 Pulkkinen, Tuija Antonio F. Rappazzo Aalto University, Espoo Bartol Research Institute University of Delaware Jack D. Scudder University of Iowa V. S. Semenov University of St. Petersburg Kazunari Shibata Kyoto University David Sibeck Goddard Space Flight Center, NASA James F. Spann MSFC/NASA Richard D. Sydora University of Alberta Karlheinz Trattner University of Colorado, LASP, Boulder Lorenzo Trenchi IFSI-National Institute for Astrophysics Dmitri A. Uzdensky CIPS, University of Colorado, Boulder Vytenis Vasyliunas Max Planck Institute Ray Walker IGPP, University of California, Los Angeles Rongsheng Wang Geophysical Institute, Chinese Academy of Sciences, Beijing, Masaaki Yamada Princeton Plasma Physics Laboratory Seiji Zenitani National Astronomical Observatory of Japan Elisabete M. de Gouveia Universidade de São Paulo, InstiDal Pino tuto de Astronomia, Geofı́sica e Ciências Atmosféricas, SP Walter D. Gonzalez Instituto Nacional de Pesquisas Espaciais, INPE, SJC, SP Pierre Kauffman Universidade Presbiteriana Mackenzie, SP Grzegorz Kowal Escola de Artes, Ciências e Humanidades (EACH), SP Iberê Caldas USP Flavia Reis Cardoso USP Instituto Nacional de Pesquisas Espaciais - INPE Finland USA USA Russian Japan USA USA Canada USA Italy USA Germany USA China USA Japan Brazil Brazil Brazil Brazil Brazil Brazil 113 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 Luı́s H.S. Kadowaki Behrouz Khiali Fernando Simões Junior Adriane Marques Raymond L. Fermo José Leonardo Ferreira Rudi Gaelzer L. F. Ziebell Adriana Válio Carlos Guillermo Giménez de Castro Marcelo Camargo de Juli Emilia Correia Francisco de Oliveira Duraes Luiz Claudio Lima Botti Sérgio Denser Pamboukian Sérgio Szpigel Marta Maria Cassiano Jean-Pierre Raulin Ricardo Yvan Ana Helena Fernandes Guimarães Albérico de Castro Barros Filho Amauri Shossei Kudaka André Luiz Garcia Pereira Antonio Luiz Basile Carlos Soncco Daneele Saraçol Tusnski Denis Pavel Cabezas Huaman Dirceu Yuri Simplicio Netto Douglas Frelix da Silva Edith Liliana Macotela Cruz USP USP UFPel INPE/DGE Boston University UnB UFRGS UFRGS Mackenzie Mackenzie Brazil Brazil Brazil Brazil USA Brazil Brazil Brazil Brazil Brazil Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Brazil Brazil Brazil Brazil Mackenzie Brazil Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Brazil Brazil Brazil Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Instituto Nacional de Pesquisas Espaciais - INPE 114 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 100 101 102 103 104 105 106 107 108 Edith Tueros Flavio de Souza Scherrer Gilmar Alves Silva Joaquim Pessoa Filho Jorge Fernando Valle Silva José Carlos Tacza Anaya Luis Olvado de Toledo Fernandes Marcio Ribeiro Gastaldi Maria Thereza Quevedo Maria Victoria Gutierrez Escate Odilon Moura Guimarães Junior Ray Fernando Hidalgo Ramirez Roberto Vitoriano Perianhes Wellington Luiz da Cruz Édio da Costa Júnior Gustavo Guerrero Olusegun Folarin Jonah Baburam Tiwari Binod Adhikar Lı́via Ribeiro Alves Odim Mendes Junior Alisson Dal Lago Maria Virginia Alves Alicia L. Clúa de Gonzalez Ezequiel Echer R. P. Kane Severino Dutra Marlos Rockenbach da Silva Claudia Vilega Rodrigues Hanumant Shankar Sawant Esfhan Alam Kherani Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Brazil Brazil Brazil Brazil Mackenzie Mackenzie Mackenzie Brazil Brazil Brazil Mackenzie Brazil Mackenzie Brazil Mackenzie Brazil Mackenzie IFMG UFMG INPE INPE INPE INPE/EMBRACE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/CRS INPE/DAS INPE/DAS INPE/DAE Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Instituto Nacional de Pesquisas Espaciais - INPE 115 Parker Workshop on Magnetic Reconnection March 18-21, 2014 - São José dos Campos, SP, Brazil 109 110 111 112 113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 128 129 130 131 132 133 134 135 136 137 138 139 140 José Humberto A. Sobral Jonas Rodrigues de Souza Daiki Koga Mariza Echer Arian Ojeda González Cristiane Loesch Rajkumar Hajra Laura Balmaceda Paulo Ricardo Jauer Fabiola Pinho Marcos V. D. Silveira Vitor Moura Suzana S. A. Silva Tardelli Stekel Jenny M. Rodrı́guez Sandra Conde Diego Barros Silva Cosme A.O.B. Figueiredo German Farinas Marisa Roberto Erico Rempel Pablo R Muñoz Emanuel Chimanski Francis Ferreira Franco Lucas Feksa Ramos Sony Su Chen Claudia Candido Paulo Alexandre Nogueira Ebenezer Chellasamy José Marques da Costa Anna Karina F. Gomes Mauricio Rosa de Souza INPE/DAE INPE/DAE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DGE INPE/DAS INPE/DAE INPE/DAE INPE/DGE ITA ITA ITA ITA ITA INPE/DGE INPE/DAE INPE/DAE INPE/DAE INPE/DAS INPE/DGE INPE/LAC INPE/DGE Instituto Nacional de Pesquisas Espaciais - INPE Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil Brazil 116

Top subcategories

Top subcategories

Top subcategories

Top subcategories

Top subcategories

Top subcategories

Top subcategories

Top subcategories

Download PARKER WORKSHOP ON MAGNETIC RECONNNECTION