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The X-Ray Telescope aboard Solar-B: An Overview

The X-Ray Telescope aboard Solar-B: An Overview. Taro Sakao (ISAS/JAXA) and The XRT Team. XRT Sciences. Imaging observation of the soft X-ray/XUV corona with advanced imaging/temperature-diagnostic capabilities. Photosphere-Corona connection

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The X-Ray Telescope aboard Solar-B: An Overview

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  1. The X-Ray Telescope aboard Solar-B: An Overview Taro Sakao (ISAS/JAXA) and The XRT Team

  2. XRT Sciences Imaging observation of the soft X-ray/XUV corona with advanced imaging/temperature-diagnostic capabilities • Photosphere-Corona connection • Formation and heating of the coronaincl. energy transport, storage, and dissipation • Outer-corona investigationextending to CME and solar wind investigations Vast varieties of active, or even non-active, phenomena in the corona:

  3. Investigation of Photosphere-Corona Connection with XRT Coronal Behavior Transient Brightenings ? Immediate Response Photospheric Magnetic Activity Time scale: minutes Spatial scale: ~1 arcsec Trigger ? ? Large-Scale Coronal Phenomena ? Eruptive flares CMEs... Reservoir ? Energy Storage Increase Spatial Scale Storage Release Time scale: days Spatial scale: ~AR SOT XRT / EIS

  4. NOAA 10314 (Emerged in a Coronal Hole region) Growing phase Mar 13 Mar 14 Mar 15 Mar 16 Large-flare-productive phase Mar 17 Mar 18 Mar 19 Mar 20 Coronal Activity Assoc. with Evolution of an Active Region (from Morita & McIntosh 2005)

  5. Two sets of dome-shaped loops Flares at “dome intersection” EIT 195Å Tiny transient sigmoid Typical Flare Evolution in the Growing Phase

  6. Sigmoid along the inversion line Flare kernel brightening Post-flare loops Typical Flare Evolution in the Large-Flare- Productive Phase

  7. Emerging bipoles into a coronal hole Flares at “dome intersection” Well-developed sigmoid structure Emergence with “two bipoles” Growing phase with occasional small flares Large-flare-productive phase • Investigate • Temperature structure of the corona (both hot & cool loops) • Pre-flare evolution leading to energy release • Long-term evolution of coronal magnetic structure • accompanying flare energy release, particularly for entire active regions • together with photospheric magnetic evolution (Morita and McIntosh 2005)

  8. Temperature Diagnostics with XRT • Optimized filter layout • Adjacent filter pairs for temperature diagnostics • SXT-like filters in one FW while TRACE-like in the other Low temperature (≦1 MK) diagnostics High-temperature plasmas XRT Advanced Features over Yohkoh SXT • Imaging/temerature-diagnositic capabilities for low-temperature (< 1MK) plasmas–Observeentire SXR/XUV phenomena in the coronaWith back-thinned CCD together with optimum focal plane filters • Highest-ever achieved angular resolution as GI imager, with wide FOV (covering the whole Sun)–1 arcsec pixel size – Cadence as high as, or even better than, SXTHigh-cadence (≦1 s) observation with small FOV available • Adjustable Focus PositionAdds variety in observations:– Highest angular-resolution (1 arcsec) for SOT/EIS FOV– Full-sun observation with 2–3 arcsec

  9. XRT Advanced Features over Yohkoh SXT • Imaging/temerature-diagnositic capabilities for low-temperature (< 1MK) plasmas–Observeentire SXR/XUV phenomena in the coronaWith back-thinned CCD together with optimum focal plane filters • Highest-ever achieved angular resolution as GI imager, with wide FOV (covering the whole Sun)–1 arcsec pixel size – Cadence as high as, or even better than, SXTHigh-cadence (≦1 s) observation with small FOV available • Adjustable Focus PositionAdds variety in observations:– Highest angular-resolution (1 arcsec) for SOT/EIS FOV– Full-sun observation with 2–3 arcsec

  10. XRT Advanced Features over Yohkoh SXT • Imaging/temerature-diagnositic capabilities for low-temperature (< 1MK) plasmas–Observeentire SXR/XUV phenomena in the coronaWith back-thinned CCD together with optimum focal plane filters • Highest-ever achieved angular resolution as GI imager, with wide FOV (covering the whole Sun)–1 arcsec pixel size – Cadence as high as, or even better than, SXTHigh-cadence (≦1 s) observation with small FOV available • Adjustable Focus PositionAdds variety in observations:– Highest angular-resolution (1 arcsec) for SOT/EIS FOV– Full-sun observation with 2–3 arcsec Telescope performance to be presented by Ed Deluca-san et al. in the next talk

  11. XRT Advanced Features over Yohkoh SXT • Improved on-board observation control by the MDP/XRT system– Automatic Exposure Control (AEC) – Automatic Region Selection (ARS) – Image-based Flare Detection (FLD; new feature) – Table-based Observation Sequence Controle.g., Exposure tracking and stabilization for AEC • Implementation of pre-flare data buffer memory inside MDP–Potentially powerful tool for detailed observation of the pre-flare corona–Investigation of pre-flare energy storage and release processes

  12. Wide-FOV Observation of Outer Corona with Diagnostic Capability on Temperature Structure 2.3 RSUN LASCO/C2 2.1 RSUN Yohkoh SXT XRT FOV for Limb Observation

  13. Wide-FOV Observation of Outer Corona with Diagnostic Capability on Temperature Structure • Frequent observation opportunity for the outer corona • Temperature structure of the corona up to 2 Rsun(c.f. Foley et al. 1997 & Wheatland et al. 1997 with Yohkoh data) • Tracking transient ejections (CMEs, filaments) in the corona 2.3 RSUN LASCO/C2 2.1 RSUN Yohkoh SXT XRT FOV for Limb Observation

  14. FOV vs Cadence Full-Sun Coverage Yohkoh SXT 1000 Full-Sun XRT Non-flare (orbit-ave.) 2” pxl size, or Q~75 (3 bit/pxl) 100 Cadence (sec) (w/ adjacent filter motion) 10 Cover SOT FOV Flare (w/o filter motion) (Hardware limit by Telescope) 1 100 1000 Observing FOV Size (arcsec) Flare Core Active Region Global Corona / Heliospheric

  15. FOV vs Cadence Full-Sun Coverage Yohkoh SXT 1000 Full-Sun XRT Non-flare (orbit-ave.) 2” pxl size, or Q~75 (3 bit/pxl) 100 Observation with Pre-Flare Buffer Cadence (sec) (w/ adjacent filter motion) 10 Cover SOT FOV Flare (w/o filter motion) ~x 3 (Hardware limit by Telescope) 1 100 1000 Observing FOV Size (arcsec) Flare Core Active Region Global Corona / Heliospheric

  16. FOV vs Cadence Full-Sun Coverage Outer corona investigation Yohkoh SXT 1000 High-cadence observation on magnetic configuraiton and temperature evolution Full-Sun XRT Non-flare (orbit-ave.) 2” pxl size, or Q~75 (3 bit/pxl) 100 Flare core with high spatial/temporal resolution Cadence (sec) (w/ adjacent filter motion) 10 Cover SOT FOV Flare (w/o filter motion) (Hardware limit by Telescope) 1 100 1000 Observing FOV Size (arcsec) Flare Core Active Region Global Corona / Heliospheric

  17. Basic Features of the XRT

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