2005/11/15STEREO/Solar-B Workshop1 Solar-B X-ray Telescope (XRT) R. Kano (NAOJ) and XRT Team XRT.

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Presentation transcript:

2005/11/15STEREO/Solar-B Workshop1 Solar-B X-ray Telescope (XRT) R. Kano (NAOJ) and XRT Team XRT

2005/11/15STEREO/Solar-B Workshop2 Solar-B Science /09/15 XRT SOT EIS “Coronal Heating” How are coronal structures heated? Dynamics in Chromosphere & Corona Coronal Activities Magnetic Activities at Photosphere

2005/11/15STEREO/Solar-B Workshop3 Targets of XRT Observations Photosphere/Corona Coupling –Can a direct connection be established between coronal and photospheric events? Coronal Heating –How do coronal structures brighten? Flare Energetics –What are the relations to the photospheric magnetic fields? CMEs, Jets and other coronal dynamical events Coronal Loop Structures & Coronal Loop Heating

2005/11/15STEREO/Solar-B Workshop4 Aschwanden et al. (1999 &2000, ApJ) SXT Loops vs. EIT/TRACE Loops Kano & Tsuneta (1996, PASJ) SXT loops in active regions highest T EIT Image Density est. from EMTemperature Isothermal Are they really different? Are they heated in a different way? We would like to observe all of the coronal plasma with a single telescope. However, we would like to distinguish between SXT loops and EIT/TRACE loops. (Importance of temperature diagnostics.)

2005/11/15STEREO/Solar-B Workshop5 Aschwanden et al. (1999 &2000, ApJ) SXT Loops vs. EIT/TRACE Loops Kano & Tsuneta (1996, PASJ) SXT loops in active regions highest EM highest T EIT Image Density est. from EMTemperature Hydrostatic Do SXT loops have a dense plasma at the top? Is it an apparent feature in a loop (by change of filling factor)? EIS can derive the coronal density with density-sensitive line pairs. (Importance of the coordinated observation between EIS and XRT.)

2005/11/15STEREO/Solar-B Workshop6 Solar-B/XRT vs. Yohkoh/SXT Solar-B/XRTYohkoh/SXT Type of OpticsGrazing Incidence FOV34 arcmin42 arcmin Pixel Size1 arcsec2.5 arcsec PSF FWHM<1 center~ 3 arcsec Bandpass3 ~ 200Å3 ~ 45Å Temp. Coverage1MK ~ 30MK3MK ~ 30MK Time Cadence Full Frame, Full-res.min 9.5sec256sec (Half Frame) Full Frame, Half-res.min 5.0sec avg. 102sec 128sec Partial Frame, Full-res. (FOV = 300”~400”) min 2.0sec avg. 15sec 8 sec in flare mode 32 sec in Quiet mode Other New ItemsPre-flare Buffer Focus Mechanism ----

2005/11/15STEREO/Solar-B Workshop7 XRT characteristics Temperature Response –TRACE-like image and SXT-like image Field-of-View and Spatial Resolution –Focus Mechanism Observation control by MDP –Table Observation –Image Compression –Time Cadences –Preflare Buffer

2005/11/15STEREO/Solar-B Workshop8 X-ray Analysis Filters XRT has 9 X-ray analysis filters and a G-Band filter. NameMetal Thickness Substrate Thickness Thin-Al/MeshAl1600 ÅMesh Thin-Al/PolyAl1250 ÅPolyimide2500 Å C/PolyC6000 ÅPolyimide2500 Å Ti/PolyTi3000 ÅPolyimide2300 Å Thin-BeBe9 µmMesh Med-AlAl12.5 µm Med-BeBe30 µm Thick-AlAl25 µm Thick-BeBe300 µm

2005/11/15STEREO/Solar-B Workshop9 XRT Temperature Response TRACE-like SXT-like

2005/11/15STEREO/Solar-B Workshop10 EIS SOT To point SOT at a certain target on the solar disk, we have to change Solar-B pointing. Therefore, XRT will not always observe the full solar disk. Many varieties of FOV size are available. Especially, for high-res.- observation, we recommend FOV= 1024”x1024” around CCD center. XRT 1024”x1024” 384”x384” 2048”x2048” Field of View (FOV)

2005/11/15STEREO/Solar-B Workshop11 Importance of Wide FOV Moreton waves tend to propagate along the global magnetic fields. X-ray waves also propagate with Moreton waves.

2005/11/15STEREO/Solar-B Workshop12 To point SOT at a certain target on the solar disk, we have to change Solar-B pointing. Therefore, XRT will not always observe the full solar disk. Many varieties of FOV size are available. Especially, for high-res.- observation, we recommend FOV= 1024”x1024” around CCD center. XRT 1024”x1024” 2048”x2048” Field of View (FOV)

2005/11/15STEREO/Solar-B Workshop13 Aberration at Different Focus Pos. ϕ 512” ϕ 1024” RMS= ϕ 1” Distance from the Center (Only Geometrical Optics)

2005/11/15STEREO/Solar-B Workshop14 Observation of XRT Mission Data Processor Observation Tables Data Recorder Image Compression Pre-Flare Buffer Autonomous Functions Exposure Control Region Selection Flare Detection XRT SOT EIS

2005/11/15STEREO/Solar-B Workshop15 Image Compression MDP can compress the image data. Observer selects the following options. –No compression –DPCM (lossless) compression –JPEG (lossy) compression Q-factor = 98, 90, …, 65.

Typical Time Cadences typical data rate for XRT ~ 600 k pixel / min –ex.1: Continuous Observation for AR AR FOV = 384”×384”, 1”-res. –ex.2: High-Speed Observation for AR AR FOV = 384”×384”, 1”-res. –ex.3: Combination of Narrow and Wide FOV Narrow FOV = 384”×384”, 1”-res. Wide FOV =2048”×2048”, 4”-res.. 40sec 3min20sec Narrow Wide 10min 50min AR 30sec AR

2005/11/15STEREO/Solar-B Workshop17 Shimojo （ ASJ 1999 autumn ） FOV = 256”x256”, 1”-res. Time Cadence = 10 ~ 20 sec for a filter pair Pre-flare Observation

2005/11/15STEREO/Solar-B Workshop18 Flare Observation XRT Detect a flare. Report the location to all telescope. XRT Intensity XRT Switch the current observation to Flare one. Lock the Pre-Flare Buffer. (There is a option not to switch to Flare obsevation.) SOT Switch the current observation to Flare one, if the flare location is in SOT-FOV. (There is a option not to switch to Flare obsevation.) EIS Switch the current observation to Flare one, if the flare location is in EIS-FOV. (There is a option not to switch to Flare obsevation.)

2005/11/15STEREO/Solar-B Workshop19 Solar-B/XRT vs. STEREO/EUVI Solar-B/XRTSTEREO/EUVI Type of OpticsGrazing IncidenceNormal Incidence FOV34 arcmin55 arcmin Pixel Size1 arcsec1.6 arcsec PSF FWHM<1 center<1.6 center Bandpass3 ~ 200ÅHe II 304Å Fe IX 171Å (1MK) Temp. Coverage1MK ~ 30MKFe XII 195Å (1.5MK) Fe XIV 211Å (2MK) Time Cadence Full Frame, Full-res.min 9.5secmin 11sec in Fe IX avg. 20min Full Frame, Half-res.min 5.0sec avg. 102sec min 4.75sec avg. 2.5min Partial Frame, Full-res. (FOV = 300”~400”) min 2.0sec avg. 15sec (No Option?)

2005/11/15STEREO/Solar-B Workshop20 Summary XRT has high sensitivity for low (1MK) temperature plasma, as well as high temperature plasma. XRT has the highest spatial resolution as GI imager. Pixel Size = 1 arcsec Observation Tables respond to various observations. Autonomous functions support XRT automatic operation. Observers can select types of Image Compression. Built-in visible light optic allows us to align XRT images with SOT images with sub-arcsec accuracy.