1 / 17

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

meena
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related