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The 6th Solar-B Science Meeting Takeo Kosugi (ISAS/JAXA, Japan) 2005 Nov. 8, Kyoto Sun - A Magnetic Star Various structures and dynamics, governed by magnetic fields The Solar Atmosphere • Coronal heating - 11-yr cycle variation • Ejections and IP disturbances - Large-scale restructuring - X-ray plasmoid - X-ray dimming (vs CME) - X-ray sigmoid (vs CME) • Solar flares as magnetic reconnection process - Soft X-ray loop-with-a-cusp structure, increasing in size with time - Double-footpoint plus above-a-loop-top hard X-ray sources - Particle acceleration site in the above-a-loop-top hard X-ray source - X-ray jets Flaring Loop and the Surroundings * Why do we need study the Sun? 1. “The Sun as a Star” (A Classical Field of Astrophysics) - Stellar Structure / Evolution - Dynamo Mechanism (Cosmic Magnetism) 2. Corona: a Prototype for Superhot Astrophysical Plasma - Why is the corona so hot? - Coronal Structure / Dynamics - Sudden Energy Release and Particle Acceleration * Key Word: Magnetic Reconnection 3. Factors Controlling the Space Weather and Climate - Solar Wind - Flares and CMEs as a Cause of IP Disturbances Science ISAS / NASA / PPARC / ESA - Coronal heating SOLAR-B - Coronal structure / dynamics - Elementary processes in Magnetic Reconnection Launch Date: Summer 2006 with ISAS M-V-7 Orbit: Sun synchronous altitude ~ 600 km Weight: ~ 900 kg Mission instruments - Optical Telescope / Vector Magnetograph (SOT) - X-ray Telescope (XRT) - EUV Imaging Spectrometer (EIS) Structure of the solar atmosphere SOLAR-B Lower atmosphere (Photosphere/Chromosphere ) governs the dynamics of the upper atmosphere (Corona) via magnetic field lines Key Elements with Solar-B Instruments • Solar Optical Telescope (SOT) Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to above 10 MK • EUV Imaging Spectrometer (EIS) Precise plasma diagnostics in the 17 – 21 nm & 25 – 29 nm ranges Continuous observation without interruption for 8 months a year Coordinated observation among the three telescopes SOT consists of OTA (Optical Telescope Assembly) and FPP (Focal Plane Package). Top door FPP: Provided by NASA/LMSAL z y x Side door Sun shade All the telescopes are complicated. SOT is just an example. Details are given in accompanying papers. Shield tube Lower Tube OTA: Provided by JAXA/NAO Mechanical Test Model (2002 May) OTA FPP EIS OBU XRT SOLAR-B SOLAR-B Thermal Test Model (2002 Oct) SOT OTA (2004 August) SOLAR-B International Collaboration SOLAR-B ISAS (Japan): Integration of S/C; Launch & Operation Mission Instruments: SOT (optics), XRT (camera), EIS (I/f to S/C) NASA (US): SOT (focal plane package), XRT (optics / mech.), EIS (optics components), NASA polar station(s) PPARC (UK): EIS (structure, detectors & electronics) ESA: Polar station(s) for data downlink Joint Operations and Data Analysis Data Usage; Proposal for Observation; etc SOLAR-B Solar-B data, together with analysis software tools, will be opened to the world solar physics (and related) communities as quickly as possible. (hopefully in a few months after data acquisition) We welcome proposals for observation plans from outside the Solar-B team. (Details TBD) Collaborative observations with other space- and ground-based observatories are encouraged. Any collaborations with, or suggestions/advices from, theoreticians are most welcome. Hinotori (1981-1982) Space Solar Physics in Japan Purely Japanese Yohkoh (1991-2001) SOLAR-B (2006) Japan – USA – UK J – US – UK – ESA (Norway) Originally prepared for COSPAR 2004 Takeo Kosugi, ISAS/JAXA