Overview of XRT Performance

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Overview of XRT Performance

• Ed DeLuca (SAO)
• with assistance from the XRT Team

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Tom Metcalf

• XRT Co-I Tom Metcalf died in a skiiing accident
  on 7-July- 2007.
• Tom worked on the XRT program from the beginning,
  he led the Lockheed Martin team that produced the
  Filter/Shutter Assembly.
• After moving to NWRA Tom continued to work with
  us as an important member of the science team. He
  was an expert in the analysis of vector magnetic
  field data and a RHESSI Co-I, in addition to
  being an XRT Co-I. His expertise is not
  replaceable.

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XRT Team

• SAO
• DeLuca
• Golub
• Weber
• Cirtain
• Lundquist
• Reeves
• Korreck
• Saar
• van Ballegooijen
• Su
• Bobra
• Jibben
• Savcheva
• Farid

• JAXA/ISAS
• Sakao
• Narukage
• NAOJ
• Kano
• Kotoku
• Bando
• NAOJ/NRO
• Shibasaki
• Shimojo

• MSU
• McKenzie
• Savage
• NWRA
• Leka
• Ishibashi
• Memphis
• Schmelz
• UNH
• Forbes
• Seaton
• Palermo
• Peres
• Reale

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Outline

• Intro to XRT
• Capabilities new features
• First Results
• Dynamics - Jets in coronal holes (and everywhere
  else)
• Topology - complex connectivity in AR, XBP fine
  structure
• Energetics - filter ratios DEMs

• Plays well with others
• XRT TRACE
• XRT EIS
• XRT SOT
• XRT SOLIS

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Intro to XRT
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The X-Ray Telescope
Mounting the XRT to the Spacecraft

• The XRT is a collaborative effort between SAO
  (mirror, filters, structure and mechanical
  systems) JAXA and NAOJ (camera sensor and
  electronics MDP software interface).
• The telescope is a modified Wolter I with a 35 cm
  aperture and a 2.71 m focal length. It has
  on-orbit focus adjustment and provides a flare
  flag to alert the other instruments.
• Properties
• Angular Resolution 1 arcsec pixels
• Encircled Energy 68 within a 2 arcsec diameter
  circle at 0.523 KeV
• Improved temperature sensitivity over the range
  from 130 MK using a back thinned 2048x2048 CCD

Length 3.0 m, Diameter 0.42 m (max), Mass 48.4 kg
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The X-Ray Telescope

• High spatial resolution
• 2.5-5 times higher than Yohkoh/SXT
• Focus adjustment allows for
• Best on axis imaging or
• Optimized imaging across a wide FOV
• Broad temperature coverage
• 1MK to 50MK
• 9 X-ray filters allow for temperature
  discrimination
• High cadence observations
• 512x512 every 30s
• Full sun every 2min
• High sensitivity
• Low thermal noise CCD
• Low scattering mirror
• Flexible operations
• Automatic Exposure Control
• Flare Detection
• Pre-Flare buffer

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Hinode XRT and Yohkoh SXT Images at a Same Solar
Activity Phase
Sakao
Hinode XRT
Yohkoh SXT
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Active Region Imaging
Yohkoh SXT
Hinode XRT
Sakao
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Quiet Regions
Hinode XRT
Yohkoh SXT
Sakao
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X-ray Bright Points
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Hinode XRT
Yohkoh SXT
2
2
3
3
1
2
2
1
3
1
3
Sakao
Bright points now resolved into ensemble of loops.
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Focal Plane Filter Wheels
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First Results
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XRT Observation Modes

• Dynamics
• Rapid evolution associated with reconnection and
  plasma instabilities - High Cadence
• Energetics
• The emission measure evolution of structures
  heating, cooling, EM changes - Multiple filters
• Topology
• Identify the magnetic connections that control
  the heating and dynamics
• Large FOV, long and short exposures

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Coronal Dynamics in XRTJets in Coronal Holes
11/23/06 Thin Al/Poly 4s. exp. 30-sec cadence,
7-hour duration
See talks by Baker today Golub tomorrow
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Long Connections in the quiet sun
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Jet outlines filament Cavity Jibben
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Flare observations See Talks by Korreck,
Shibasaki and Seaton on 23-Aug Poster by Reeves.
SOT-FG/Ca H (color) XRT (contour)
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Narukage 24-Aug
XRT Energetics Filter ratios - a new usage
Log(EM)
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Reale, Parenti (Reale Tomorrow) Thermal map from
5 filters
Test of Reale et al. multi filter technique on
flares. Parenti Poster
Blue marks the saturated pixels. The T varies
between 6.1 and 6.9 in LogT.
1056
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Schmelz AR DEM Analysis
DEM from the 11 filters/filter combinations data
set from 13 May 2007. Flux from limb active
region has been summed in a 1 arcmin x 1 arcmin
square. Best fit DEM reveals a superhot
component at Log T 7.5, but 100 realizations
show that this component may not be real. Long
exposures in thick XRT filters are required to
confirm this suggestive result.
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Reeves Poster, DEM analysis of post flare loops
from seven X-ray filters. 2007-07-10 - C8.2 Peak
1240
1320
1310
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Magnetic feature and morphological study of X-ray
bright points
Magnetic footpoints did not seem to move although
X-ray intensity changed.
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XRT Topology Observations of a Coronal
Sigmoid(See Golub Tomorrow)

• McKenzie, Canfield

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• Coronal Magnetic Structure - NLFFF
• Bobra Lundquist

12 December 2006
161257 UT
Left XRT Al/Poly image. Middle Selected field
lines from the models result. Right
Quasi-separatrix layers (white) derived from
models result.
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Plays Well With Other Instruments
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TRACE and XRT are Complementary
TRACE 11/13/06
XRT 11/13/06
Golub
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B vs. X
MDI Magnetogram
XRT Ti_poly , 1 sec., 11/04/06
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XRT Will Combine With SOT for Photosphere/Corona
Connectivity Studies
XRT v. SOT G-band 11/14/06 B bifurcation over
light bridge
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XRT will combine with EIS for powerful diagnostics
EIS 40 Slot
??? XRT ??
XRT
Fe XV 284
He II 256
EIS Spectrum
??(nm)
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XRT, EIS TRACE co-observe the 17-Dec-2006 limb
flare
EIS (1 of 9 strong lines)
XRT with TRACE Contour
TRACE
Hara Reeves
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13-May-2007 SOLIS Photospheric Chromospheric
magnetograms XRT Al_poly/Ti_poly
Weekly program during EIS 3.5hr disk center
calibration SOLIS Photospheric Vector or LOS
magnetograms Chomospheric LOS
magnetograms XRT Multi-filter full sun full
resolution image Goals Studies of the
relationship of magnetic topology and coronal
energitics, for QS, AR, CH
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Working with Hinode

• Chief Coordinators
• John Davis (john.m.davis_at_nasa.gov)
• Tetsuya Watanabe (watanabe_at_uvlab.mtk.nao.ac.jp)
• Science Schedule Coordinators
• SOT T. Berger (berger_at_lmsal.com),
• XRT L. Golub (golub_at_cfa.harvard.edu)
• EIS J. Mariska (mariska_at_nrl.navy.mil)
• XRT Observing (XOB) Proposals http//solar.physic
  s.montana.edu/HINODE/XRT
• XRT USERS Email List
• Send mail to xrt_users-request_at_head.cfa.harvard.ed
  u

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THREE DATA ARCHIVES
http//sot.lmsal.com/sot-data
http//darts.isas.jaxa.jp/hinode/
http//kurasuta.cfa.harvard.edu/VSO
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End