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Solar-C X 線 /EUV 望遠鏡

Solar-C X 線 /EUV 望遠鏡. 坂尾太郎 JAXA 宇宙科学研究所. The Solar-C Mission. Fourth Japanese solar physics mission following Hinode , with anticipated launch in late 2010’s. A set of three telescope instruments: SUVIT – Large (~1.5 m f mirror) optical telescope

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Solar-C X 線 /EUV 望遠鏡

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  1. Solar-C X線/EUV望遠鏡 坂尾太郎 JAXA宇宙科学研究所

  2. The Solar-C Mission • Fourth Japanese solar physics mission following Hinode, with anticipated launch in late 2010’s. • A set of three telescope instruments: • SUVIT – Large (~1.5 mf mirror) optical telescope • EUVST – UV/EUV high-throughput spectrometer • XIT – X-ray imaging (spectroscopic) telescope • With seamless coverage of the entire solar atmosphere and with spectro (-polarimetric) measurement capability, identify magnetic field structure and reveal mechanisms of heating and dynamic activities in the solar atmosphere. • Extensive international collaboration with ESA and NASA anticipated. EUVST SUVIT (S/C: ~6.7m in height, ~3.5m in bus module width) XIT

  3. Key Hinode Observations Relevant to Solar-C • Dynamic chromosphere, with activities protruding even into the corona.Chromosphere may be playing a key role for the heating of the outer atmosphere.* Need of understanding vector magnetic field structure of the chromosphere. • Possible sub-arcsec non- thermal events ongoing at the footpoints of coronal loops. Contribution to coronal heating? Corona (Movie courtesy of Y. Katsukawa) • Something crucial resides in angular scales within our reach in the chromosphere/ lower corona. • Power of imaging spectroscopy.

  4. Imaging Observation of the Corona TRACE 171Å EIS 195Å EIS 284Å SXR (XRT) Causal connectivity between the base of the corona and the chromosphere/transition region with EUV-line images Heating and activities of hot loops with broad-band soft X-ray images • Normal Incidence (Baseline) • Ultra-high-resolution with high-cadence imagery in EUV wavebands • Connectivity with lower atmosphere • Context information for EUVST • 0.2-0.3” angular resolution (0.1”/pixel) with cadence <10 s for AR/FL • 171, 94 and 304 (or 1548 UV) Å bands • Grazing Incidence (Optional) • Highest spatial-resolution soft X-ray imaging-spectroscopy • Photon-counting capability for reconnection structure etc. • ~< 1” angular resolution (0.4-0.5”/pxl) • ~0.5-10 keV energy range

  5. MHD structure and particle acceleration assoc. with magnetic reconnection Connecting low corona and chromosphere AIA 193Å NST He I 10830-0.25Å Identification of supra-thermal (non-thermal) electrons with energy range up to ~10 keV Ji, Cao, and Goode 2012, ApJ - BBSO/NST He I 10830Å - SDO/AIA 171 Å Structure with diameter ~100 km

  6. Fine Structures in the Corona Hi-C Experiment (July 2012) AIA 0.6” pixel vs Hi-C 0.12” pixel (Courtesy J. Cirtain)

  7. High Resolution Imagery of the Corona Coronal heating by reconnection Braiding structure as a possible agent for coronal heating? (Cirtain et al. 2013)

  8. High Resolution Imagery of the Corona Coronal heating by waves Contribution of high- frequency waves? - Low freq. (P >~ 100 s) not likely to heat ARs (McIntosh et al. 2011) - How about P down to ~10s ? 304 Å 171 Å 304 Å 171 Å Role of chromospheric spicules into the corona Image fine structures predicted by numerical simulations (Martinez-Sykora et al. 2011)

  9. Line Candidates (Provisional) (Viall & Klimchuk 2012)

  10. Preliminary Outlook of the X/EUV Telescope NI Secondary Mirror NI Primary Mirror GI Segment Mirror Baseline 3 NI Channels: 94, 171, 304 Å (or 1548 Å) Sector coating Optional GI Channel: Photon Counting in 0.5-10 keV

  11. Three-Channel NI Layout (Figure courtesy of SAO) 171Å 94Å 304Å Primary: Φ32 cm, efl=16 m Sector: Ageom≈ 100, 200, 300 cm2 Channel selection via focal plane filters!

  12. Preliminary Features of XIT-NI • Image • Lower TR • Lower corona • Hot corona (with 1 MK) Provide context for EUVST

  13. Science Targets of the GI Telescope (Photon-Counting) • Energy dissipation processes in the corona that lead to dynamic activities of the corona. • MHD structures assoc. with magnetic reconnection during flares • Identify, e.g., shock structures (slow shock, fast shock) • Plasma conditions (temperature, heating status) in the upstream/downstream regions of a shock • Electron temperatures from continuum spectra • Spatial distribution and evolution of supra-thermal electrons(which serve as the seed for accelerated electrons) • Heating mechanism for active regions • In particular, for hot plasmas in the AR core: • Spatial and temporal evolution of spectra with high time resolution by virtue of non-dispersive imaging-spectroscopy* Particularly powerful under the nano-flare-heating picture for ARs. • Spatial distribution of spectral features (Disk AR・・lateral, Limb AR・・・vertical）

  14. Possibilities:Shocks in the Reconnection Structure Energy range covering up to ~10 keV should clearly identify presence of supra-thermal electron components e- distribution spectra outside diffusion region Supra-thermal electrons Thermal electrons 10 keV e- distribution spectra around reconnection point Imada et al. JGR 2011 (Tsuneta,Ap.J.1996) (Tsuneta,Ap.J.1996) Electron acceleration at Earth’s magnetotail (Tsuneta,Ap.J.1997)

  15. Key Features of the Photon-Counting Soft X-ray Telescope

  16. Backup Slides

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