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HINODE/X-Ray Telescope

HINODE/X-Ray Telescope. Golub et al. “The X-Ray Telescope (XRT) for the Hinode Mission” 2007, Solar Physics , 243, pp. 63-86 Kano et al. “ The Hinode X-Ray Telescope (XRT): Camera Design, Performance and Operations ” 2007, Solar Physics , in press. R. Kano （ NAOJ ） & Japan-US XRT Team.

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HINODE/X-Ray Telescope

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  1. HINODE/X-Ray Telescope • Golub et al.“The X-Ray Telescope (XRT) for the Hinode Mission”2007, Solar Physics, 243, pp. 63-86 • Kano et al.“The Hinode X-Ray Telescope (XRT): Camera Design, Performanceand Operations”2007, Solar Physics, in press. R. Kano （NAOJ）& Japan-US XRT Team Hinode Workshop in China

  2. Hinode Solar Optical Telescope: SOT ３望遠鏡の同時観測により、 太陽コロナ活動や加熱機構のメカニズムを探る 0.2-0.3秒角という超高空間分解能で、太陽表面の磁場ベクトルを精密計測 EUV Imaging Spectrometer: EIS コロナの物質が出す極端紫外線を撮像・分光し、コロナ物質の密度・温度・流れの状態を診断 X-ray Telescope: XRT 約１秒角の高解像度で、コロナの構造やそのダイナミックな変動を観測 Hinode Workshop in China

  3. Outline • Introduction of X-ray telescope • Control of XRT observations • Coronal temperature diagnostics • Summary Hinode Workshop in China

  4. 1. Introduction of XRT Hinode Workshop in China

  5. This is XRT Graphite Tube Assembly CCD Camera and Radiator Ascent Vents 2 places NAOJ ISAS SAO Electrical Box Front Door and Hinge Assembly Hinode Workshop in China

  6. This is XRT Optimized set of focal-plane filters Sophisticated observation control by MDP Graphite Tube Assembly CCD Camera and Radiator Ascent Vents 2 places Electrical Box Back-Illuminated CCD: 2k x 2k pixel Front Door and Hinge Assembly Grazing Incidence X-ray Mirror Hinode Workshop in China

  7. XRT Optics • Grazing incident X-ray optics. • Visible light (G-band) optics on the central axis shears one CCD with the X-ray optics, and its images are used for the co-alignment with SOT Hinode Workshop in China

  8. moderate resolution for wide FOV high resolution in narrow FOV Optical Performance Point Spread Function • Increased spatial resolution while maintaining FOV covering the whole Sun • ~3 times higher (1 arcsec pixel size) than Yohkoh/SXT= highest ever achieved for soft X-ray telescopes for the Sun. • Focus adjustment mechanism • Imaging with the highest resolution for areas covering SOT/EIS field of view. • Or, full-Sun imaging with a moderate (2 - 3”) resolution. XRTSXT ※SXT @ Al K (8.34A) XRT @ Cu-L line(13.3A) Hinode Workshop in China

  9. XRT analysis filters • XRT has 9 X-ray filters and 1 visible light filter. Thin-Be G-band Med-Be C-Poly Thick-Al Ti-Poly Thin-Al-Poly Thin-Al-Mesh Med-Al Thick-Be open open Hinode Workshop in China

  10. XRT analysis filters Optimized filter selection and layout • Adjacent filter pairs for temperature diagnostics. • Both SXT-like and TRACE-like filters included in the set. Hinode Workshop in China

  11. Key features of XRT • Continuous coverage of the entire temperature range in the corona for ≳1 MK plasmas … Capable of observing entire plasma processes that take place in the corona, with temperature diagnostic capability • High angular-resolution/contrast observations for high temperature (≳2 MK) plasmas Hinode Workshop in China

  12. Hinode/XRT (Full Sun) Scientific Location of XRT (Angular resolution and temperature range) Yohkoh/SXT (Full Sun) Temperature range ～2 MK SoHO/EIT (Full Sun) TRACE (Partial) Angular resolution (CCD Pixel Size) 2.5” 1” 0.5” Hinode Workshop in China

  13. Hinode XRT and Yohkoh SXT Imagesat a Same Solar Activity Phase Spatial resolution 1 arcsec 5 arcsec Hinode XRT Yohkoh SXT Hinode Workshop in China

  14. Active Region Hinode XRT Yohkoh SXT Hinode Workshop in China

  15. Quiet Region Hinode XRT Yohkoh SXT Hinode Workshop in China

  16. X-ray Bright Points 1 2 Hinode XRT Yohkoh SXT 2 3 3 1 2 2 1 3 1 3 Bright points now resolved into ensemble of loops. Hinode Workshop in China

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

  18. 2. Control of XRT observations Hinode Workshop in China

  19. Mission Data Processor Observation Tables XRT SOT DR Image Compression Data Packet Edition Pre-Flare Buffers EIS Autonomous Functions AEC ARS FLD On-board functions for XRT Obs. Mission Data Processor (MDP) has many functions for XRT. • Management of XRT exposures by “Observation Table” • Autonomous Functions for XRT observations • Automatic Exposure-duration Control (AEC) • Automatic Region Selector (ARS) • FLare Detection (FLD) • Image processing • Edition of Image data packets • Image compression • Pre-Flare Buffers Hinode Workshop in China

  20. Observation Table • XRT exposures are managed by one observation table in the Mission Data Processor (MDP). • The structure of XRT observation table is essentially the same with those for SOT. Observation Program (20 programs) Sequence Table (100 sequences) • Program No.1 • “Normal Obs.” • SUB1loop=10 • SUB3loop=1 • SUB2loop=10 • SUB3loop=1 • SEQ1: global structure of 1MK corona • Exp. for thin-Al-mesh & full FOV • Exp. for thin-Al-poly & full FOV • SUB1 • SEQ1loop=1 • SEQ2loop=20 • SEQ2: AR’s temperature structure • Exp. for thin-Al-poly & small FOV (AR) • Exp. for med-Be-mesh & small FOV (AR) • SUB2 • SEQ1loop=1 • SEQ3loop=20 • SEQ3: 1MK corona in AR • Exp. for thin-Al-mesh & small FOV (AR) • Exp. for thin-Al-poly & small FOV (AR) • SUB3 • SEQ100loop=1 ： SEQ100: CCD dark calibration Hinode Workshop in China

  21. Automatic Exposure-duration Control (AEC) Over Exposure Exposure duration is adjusted by using the intensity histogram. Number of pixel LLTULT F(I) If U is too much, shorten the exposure duration. IntensityI Normal Exposure Number of pixel LLTULT F(I) If L is not enough, lengthen the exposure duration. IntensityI Under Exposure Number of pixel LLTULT F(I) Hinode Workshop in China IntensityI

  22. Automatic Region Selector (ARS) • XRT will take an “ARS patrol image” (the full CCD-frame and 2”-resolution) once per orbit (every 90 min typically). • Two modes of ARS run in parallel each other. • “Global Search”mode to fine the brightest region. • “Local Search”mode to track bright regions. Hinode Workshop in China

  23. ARS: Global Search Steps to derive a new FOV • Take a new patrol image. • Define the search area.(The default is all CCD.) • Make a macro-pixel image. • Pick up the brightest macro-pixel. • Calculate a fine position in the original image around the selected macro-pixel. New FOV Hinode Workshop in China

  24. Automatic Region Selector (ARS) • XRT will take an “ARS patrol image” (the full CCD-frame and 2”-resolution) once per orbit (every 90 min typically). • Two modes of ARS run in parallel each other. • “Global Search”mode to fine the brightest region. • “Local Search”mode to track bright regions. Hinode Workshop in China

  25. ARS: Local Search Steps to derive a new FOV • Take a new patrol image. • Define the search area.(Just around the current FOV) • Calculate a fine position in the search area. Current FOV New FOV New FOV Hinode Workshop in China

  26. Flare Detection (FLD) • XRT will take a FLD patrol image every 30 sec (typically). • MDP derives a difference image between a new patrol image and the running averaged patrol image, and searches any intensity enhancement in it. • Once a flare occurred, MDP informs the flare position to SOT and EIS also. • (FLD function is useful to avoid strong irradiation to CCD.) FLD patrol image FLD patrol image FLD patrol image 30 sec (typically) 30 sec (typically) Averaged image Averaged image Averaged image Averaged image average average average difference difference difference Flare has detected! Flare is lasting. Flare has terminated. Hinode Workshop in China

  27. Pre-Flare Buffers Four buffers is available for the image transfer to the Data Recorder. • Buffer0 is prepared for the normal image transfer. • Buffer1, 2, and 3 for ring buffers to freeze the pre-flare images. Buffer0 Data Recorder Buffer1 “SW3” “SW1” Buffer2 Buffer3 “SW2” Total time X X−300s X−200s X−100s Buffer0 Hinode Workshop in China Buffer1 Buffer2 Buffer3

  28. Mission Data Processor Observation Tables XRT SOT DR Image Compression Data Packet Edition Pre-Flare Buffers EIS Autonomous Functions AEC ARS FLD On-board functions for XRT Obs. Mission Data Processor (MDP) has many functions for XRT. • Management of XRT exposures by “Observation Table” • Autonomous Functions for XRT observations • Automatic Exposure-duration Control (AEC) • Automatic Region Selector (ARS) • FLare Detection (FLD) • Image processing • Edition of Image data packets • Image compression • Pre-Flare Buffers Hinode Workshop in China

  29. Parameters of XRT Performance Hinode Workshop in China

  30. 3. Coronal temperature diagnostics Hinode Workshop in China

  31. Spectrum of Solar Corona Spectrum of the solar corona is modeled as an optically thin plasma, and consists of a continuum and emission lines. XRT is a sensitivity around 150-200Å to observe a low temperature corona (100MK). Hotter plasma is brighter in short wavelengths. Hinode Workshop in China

  32. XRT analysis filters • XRT has 9 X-ray filters and 1 visible light filter. Thin-Be G-band Med-Be C-Poly Thick-Al Ti-Poly Thin-Al-Poly Thin-Al-Mesh Med-Al Thick-Be open open Hinode Workshop in China

  33. Nine X-ray filters. Wide-wavelength coverage. XRT Response (Effective Area) To observe 100MK plasma, XRT has a sensitivity at 170 – 200Å with thin-Al-mesh. Hinode Workshop in China

  34. Coronal spectrum at a certain logT × XRT effective area ＝ A wavelength distribution of the coronal intensity with logT detected with XRT. We derive a total intensity of the corona at logT detected with XRT, by integrating it over wavelengths. By plotting total intensities at several temperatures, … we derive a “temperature response: ffilter(T)”. x = Coronal Intensity detected with XRT * Hinode Workshop in China

  35. filter ratio method Hinode Workshop in China

  36. filter ratio method • Filter ratio method Assumption : XRT observe same plasma with filter1 and filter2. The estimated temperature is themean temperature. filter ratio function Hinode Workshop in China

  37. Temperature Diagnostics with XRT Low-Temperature Structure around an AR Hinode Workshop in China

  38. 4. SUMARRY (1) • XRT holds a unique position among solar SXR/EUV telescopes currently on orbit or being planned:* Continuous coverage of the entire temperature range in the corona for ≳1 MK plasmas … Capable of observing entire plasma processes that take place in the corona, with temperature diagnostic capability* High angular-resolution/contrast observations for high temperature (≳2 MK) plasmas • Autonomous functionsto support various observations of coronal dynamics. Hinode Workshop in China

  39. 4. SUMARRY (2) • Structure and evolution of coronal magnetic fields and their associated temperatures can be investigated in great detail. • Expected to serve as a key instrument for investigating photosphere-corona connection. At the same time, may have non-negligible impact on heliospheric study. Hinode Workshop in China

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