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F2B: Quantify Particle Acceleration for Key Regions of Exploration Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction Production and distribution of the seed particles (pickup ions, suprathermal plasmas in the solar corona and planetary magnetospheres) that are accelerated to high energies Required Understanding Identify dominant processes controlling stochastic acceleration Quantify the dynamics of magnetic topology and electric fields in key regions Quantify the critical parameters that drive acceleration phenomena across shock boundaries Determine the role of parallel DC electric field, Alfvén and low frequency waves in acceleration process Enabling Capabilities & Measurements Remote and in situ particle and field observations of the corona and nearSun acceleration regions Models to quantify the interaction of multiple acceleration mechanisms in key regions Great Observatory Assumes launch of Solar-B, MMS, SDO, RBSP, THEMIS, IBEX, Cluster, ITSP, L1 monitor Enabling LWS missions SEPP - quantify critical parameters for the source regions and the SEP outputs Contributing LWS Program Sentinels – will observe heliospheric acceleration shock regions created by CMEs Contributing STP Program GEC– measures ionospheric control of magnetospheric acceleration processes Hybrid computer algorithms focused on shock region models in key regions In situ and remote high temporal, spectral and spatial resolution observations in connected acceleration regions in nearEarth region Spatially and temporally resolved observations of shock interface in key regions (Sun-Corona, SW-CME-CIR, CME-Mag, Helio-Interstellar) Implementation Phase 2: 2015-2025 Enabling STP Program AAMP – mission to quantify the acceleration processes probing the readily available near Earth environment. Enabling STP Program IMC – mission to quantify the acceleration processes in the inner magnetosphere Contributing STP Program MTRAP - mission to explore the solar acceleration region dominated by magnetic pressure Enabling Contributing Model/Theory Development - What resource SPI/Telemechus - understand solar dynamo - put in phase 3 instead? Flagship mission Solar Probe – will provide obs of acceleration process near sun Community wide modeling workshops focusing on model development + Theory Program Potential Discovery Mission to observe in situ and quantify interplanetary acceleration processes at shock boundaries Potential Explorer Mission to observe and quantify acceleration processes associated with electric field in a magnetized environment Other Agencies US: L1 Monitor, ATST Foreign: ORBITALS, Ravens, Solar Obiter 1 F2C: Quantify Coupling Mechanisms at Critical Interfaces Targeted Outcome: Phase 2- 2015-2025, Open the Frontier to Space Environment Prediction Transfer of solar wind information through planetary electrodynamic systems Required Understanding Feedback of the ionosphere on magnetospheric electrodynamics Meteorological Forcing of the ITM Chemical & dynamical coupling between upper atmosphere disturbances & the lower atmosphere Detailed coupling of magnetotail dynamics to the polar region Controllers of mass and energy flow between the solar wind and geospace Transition of solar steady and eruptive events from interior of the sun to the atmosphere Global I-T coupling and the creation of instabilities Enabling Capabilities & Measurements Simultaneous, colocated neutral winds, ionospheric densities & drifts Global characterization of the current systems linking geospace using swarms of satellites Simultaneous multi-point characterization of the magnetotail and imaging of the auroral oval Satellite observations of atmospheric chemistry & key dynamical features Two-way-coupled modeling capabilities Multi-point measurements of solar wind and dayside magnetopause Simultaneous measurement of solar reconnection features and heliospheric density structures Implementation Phase 2: 2015-2025 MMS, ITSP, RBSP, SDO The existing Great Observatory provides necessary measurements to understand the linkages ITM-Waves, GEC, GEMINI, MC, Sentinels These are the most important missions in this phase to address coupling mechanisms at interfaces Mars Dynamics interface between the upper and lower atmosphere at Mars Solar Probe, SEPP, MTRAP, DBC, AAMP, SPI/TLM Theory/Modeling Coupled models between regions of space to provide physical insight on mass and energy transfer rates These are missions that also could provide critical measurements for understanding linkages between regions 2 J2A: Characterize the Near-Sun Source Region of the Space Environment Phase 2015-2025, Safeguard the Outward Journey Particle acceleration mechanisms in CME shocks and CME/flare current sheets Relationship between CME evolution and pre-existing solar wind conditions Link the solar disturbances to their geoeffective consequences UV Spectroscopic determination of Pre/Post-shock density, speed, compression; ion/ electron velocity distributions, charge states, abundances; Alfven speed, magnetic field, reconnection rates in CME shocks, flares, current sheets Required Understanding Recognition of precursors of large CMEs, flares and SEP events responsible for major space weather disturbances Link between magnetic field and solar wind at all latitudes SOLAR-B, SDO, SENTINELS STP and LWS missions from previous phases Relationship between magnetic flux emergence & transport and the solar wind Understand solar reconnection through the planetary analog Enabling Capabilities & Measurements Multipoint Visible light observations of Coronagraph/ magnetospheric Polarimeter for reconnection electron density and evolution and reconfiguration flow speeds High latitude observations of fields & particles Implementation Phase 2: 2015 - 2025 Assumed Phase 1 Assets Acceleration mechanisms and sources of the fast and slow solar wind Enabling Program LWS SEPP to fully characterize coronal sources of SEPs, CME shocks and current sheets Contributing Program ? Mars Aero. Probe to understand Solar reconnection through the Mars analog Enabling Near-Sun in situ measurements of charged particle distribution, composition, waves & fields; neutrons, hard Xrays & gamma rays LWS Program MagCon, AAMP, GEMINI to understand Earth analog to Solar reconn. and determine geospace effects of Solar sources Enabling LWS Program Doppler to identify disk signatures of CME, flare, and SEP initiation On-Disk UV/EUV Spectrographic imaging for Geospace flow velocities, energy observations release signatures; Disk to quantify effects of Magnetograph for magnetic solar sources field topology and evolution Contributing Enabling Flagship Mission Solar Probe for in Partnership Solar Orbiter for in situ sampling of inner heliosphere situ sampling of inner heliosphere Contributing STP Program SPI or Telemachus To characterize high latitude source regions Integrated empirical Theory/Modeling Program To guide the evolution of physics based predictive theory 3 J2C: Determine Mars Atmospheric Variability Relevant to Aerocapture, Entry, Descent, Landing, Surface, Navigation and Communications – Phase 2015-2025, Safeguard the Outward Journey Required Understanding Wave-wave interactions at all scales Non-LTE radiative transfer Dust, aerosol evolution and characteristics Simultaneous and coordinated global measurements of neutral & plasma density, B-field, temperature, winds Neutral & plasma instabilities Waveturbulence interactions Plasma-neutral coupling with B-field Lightning To inform on tidal and tide-mean flow processes relevant to Mars Wave-mean flow interactions Enabling Capabilities & Measurements Critical Regimes: Entry, Descent & Landing (EDL), 0-40 km; Aerocapture, 40-80 km; Aerobraking & Orbital Lifetime, 80-250 km; Ionosphere 90-200 km Electrical & Dust Environments Empirical models of global Mars atmosphere structure & variability Implementation Phase 1: 2005-2015 CNOFS, TIMED Mission Plasma irregularities at Earth & Mars & effects on radio propagation Parameterizations of turbulence and gravity wave effects in GCMs LWS Program IT Storm Probes + ITImager Mission To inform on plasma irregularities relevant to COMM and NAV systems at Mars and between Earth & Mars Mitigate ionosphere effects on precision landing (GPS) Implementation Phase 2: 2015-2025 Potential Scout ITM WAVES Theory & Mars Dynamics Mission Modelling To inform on waveMission wave, wave-mean flow To collect observations of Program processes and What Program? parameterizations relevant to Mars Theory & Modelling Program To understand waves, instabilities, and plasma processes that determine variabilities of Earth & Mars’ environments; develop surface to ionopause first-principles model of Mars’ atmosphere First principles data-assimilating models for predicting global atmosphere and ionosphere structure densities, temperatures and winds 0-100 km over all local times at Mars GEC Dipper mission, Earth analog to dynamics and variability of the lower thermosphere To develop an Assimilative Model for Mars’ whole Atmosphere 4 F3A: Predict Solar System Magnetic Activity and Energy Release Targeted Outcome: 2025-beyond, Opening the Frontier Dominant processes controlling solar dynamo Characterize predictability of dynamo: analytic, statistical, or chaotic Required Understanding Solar surface and interior flows as drivers for solar magnetic field evolution on active region, solar cycle and century time scales Dominant processes controlling magnetic structuring, energy buildup, storage, and release Characterize predictability of magnetic energy release Production of paleoclimate tracers of solar activity Understand to the level of predictability the ionospheric dynamo Whole-Sun remote-sensing observations (magnetic, velocity, XUV, EUV) Enabling Capabilities & Measurements Global heliosphere in-situ observations (plasma, field, particles) Measurements throughout the magnetosphere of fields and particles Measurements throughout the ionosphere and thermosphere of density, comp. and drifts Active region coronal measurements of magnetic field, velocity, thermal fine structure Integrated solar interioratmosphere magnetic models using observational inputs Integrated MHD/plasma models of coronal magnetic heating and stability Implementation Enabling: Enabling: SHIELDS, SPI, Farside - remote sensing MagCon: magnetotail dynamics SWB, SPI - in-situ IMC: inner magnetospheric dynamics RAM, MTRAP - coronal structure DBC: dayside magnetic structure Enhancing: Stellar Imager – dynamo context Theory and Modeling: Predictability analysis of MHD systems 5 F3B: Predict High Energy Particle Flux Throughout the Solar System Targeted Outcome: Phase 3- 2025-beyond, Opening the Frontier From Phase 2: Understand SW magnetic processes and quantify acceleration in key regions Understand the transfer of energetic particles between regions of space (e.g., heliosphere to magnetosphere) Required Understanding Understand the source of dominant processes that create energetic particles at the Sun, in interplanetary space and within magnetospheres Understand transport processes of energetic particles in interplanetary regions in the Solar System Understand the energization processes across multiscalar interfaces that result in acceleration of particles Determine the plasma populations throughout the Solar System Enabling Capabilities & Measurements Remote and in situ particle and field observations of key regions where energetic particles are generated Develop physics based models that predict particle fluxes within magnetospheres In situ observations of plasmas within .5 AU that will Remote and in situ observations in Geospace and other planetary magnetospheres in order to predict particle fluxes Develop physics based models that predict particle fluxes out to 1.5 AU using solar and innerheliospheric observations Great Observatory Assumes launch of ITSP, L1 monitor, SEPP, Auroral Imagers, Solar Sentinels, MTRAP, solar chronograph Flagship mission Potential Discovery Mission to observe quantify Mercury’s magnetospheric particle and plasma populations Mission to quantify the particle and energy propagation through the solar wind-magnetosphere-ionosphere system IMC, MagCon, DBC, AAMP Potential Explorer Mission to quantify the dynamics of and particle interaction across the heliospheric boundary Implementation Phase 3: 2025-beyond Enabling LWS missions Solar wind mission that quantifies particle fluxes within 1 AU and within Geospace Contributing LWS Program Mission that remotely observes the solar source of particles and impact of particles in Geospace Enabling STP Program Mission to observe the far side of the Sun Contributing STP Program Mission to remotely investigate extraterrestrial magnetospheres Contributing ??? Program Interstellar Probe - Measurements during cruise phase Enabling Model/Theory Development Theory and Modeling program focused on predicting particle flux and populations throughout the Solar System Other Agencies US: monitor of geoeffective solar phenomena (chronograph?) 6 F3C: Understand the Interactions of Disparate Astrophysical Systems Targeted Outcome: Phase 3- 2025-beyond, Open the Frontier Required Understanding Cosmic ray interaction with heliopause Understand to the level of prediction the coupling between interplanetary medium and magnetosphereionosphere-atmosphere system Image heliopause Enabling Capabilities & Measurements Image termination shock using energetic hydrogen atoms and radio detection Multipoint measurements of SWmagnetosphere coupling Heliospheric Imager & Galactic Observer (HIGO) To image the interaction between interstellar medium and heliopause Physical structure of bow shocks (termination shock) at heliopause, supernova remnants, binary star interaction regions, neutron star spheres, and black hole horizons. Cross-scale coupling of galactic magnetic field between interstellar medium and heliosphere The location and 3D structure of the interaction region between the heliosphere and local galactic environment Determine isotopic and elemental composition, flow directions, speed, and temperature of pickup ions and neutrals with in-situ stellar probes In situ and remote measurements of magnetosphere-ionosphere coupling Measure low-energy cosmic rays in situ with interstellar probes Solar sail technology to enable interstellar spacecraft Measurements of coupling between atmospheric layers/regions Implementation Phase 3: 2025-2035 Interstellar Probes, Explorers & Missions To explore interstellar medium Stellar Imager To explore the magnetic activity of other stars Theory/Modeling Program To simulate shock waves in astrophysical environments DBC, MagCon, IMC TITM-C, ITM-Waves, AAMP Constellations to investigate SWmagnetospheric coupling Missions to quantify atmospheric coupling 7