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Title: Hinode XRT: An Overview


1
Hinode XRT An Overview
  • M. Bobra
  • Harvard-Smithsonian Center for Astrophysics
  • Cambridge, MA
  • With contributions from the XRT Team
  • (SAO, NASA, JAXA, NAOJ)
  • and additional contributions from
  • the EIS team (STFC, NRL, JAXA, NAOJ)
  • and the SOT Team (NAO, LMSAL, NAOJ, JAXA)

2
First X-Ray Image of the Sun
X-ray/EUV emission from flares suspected in
1950s -- Ellison, 1950, Pub. Royal Obs,
Edinburgh deduced EUV emission from effect on
ionosphere -- Chubb, Friedman, Kreplin,
Kupperian, 1957, Nature, 179, 861 7 years of
rocket observations, 5 X 10-3 ergs/s/cm2 from
quiet sun
-- Giacconi et al., 1965, ApJ, 142, 1274 --
spatially highly structured corona
3
Skylab, 1975
Leon Golub
4
Rocket Flight NIXT, 1992
5
Yohkoh, 1991 - 2005
grazing incidence, 2.5 MK, monitoring through a
cycle
6
The Hinode Spacecraft
  • Hinode is a Japanese mission with contributions
    from the USA, UK and Europe.
  • SOT A high resolution optical telescope that
    provides spectrally resolved images, Dopplergrams
    and vector magnetograms
  • XRT A high resolution X-ray telescope that
    provides coronal temperature and density maps
  • EIS An EUV imaging spectrometer that provides
    spatially resolved high resolution spectra.

Uchinoura Space Center Kagoshima, Japan
7
Hinode Spacecraft Properties
  • Mass 875 kg
  • Power 1000W
  • Telemetry 4 Mbps
  • Data Recorder 8 G bit
  • Attitude Solar pointed
  • Stability 0.3 arcsec per 1s
  • Launch 23 September 2006
  • Orbit Polar, Sun-Synchronous, 600km

8
Comparative Fields of View
9
Automatic Tracking
Hinode can select and track any region on the Sun
Limb viewing
Change to new target
Polar Observation
Spacecraft pointing targets determined every
morning
10
Solar Optical Telescope
  • Telescope
  • F9, aplanatic,Gregorian with a 50 cm aperture.
  • Diffraction limited performance 388-670 nm
  • Angular resolution is 0.2 at 400 nm
  • The field stop restricts the FOV to 4x4 arcmin2
  • The OTA also contains the polarization modulator
    for the magnetographs and the tip/tilt mirror for
    the Correlation Tracker

11
Completed Optical Telescope Assembly
12
The Focal Plane Package
The FPP contains three instruments a
spectropolarimeter, a broad band imager and a
narrow band imager Dimensions 1.63 x 0.65 x 0.37
m3 Mass 48.4 kg
  • The Spectropolarimeter (HAO) records full Stokes
    profiles of the magnetic field
  • Slit Width 1.6 x 164 arcsec2
  • Spectral Range 6302.05Å
  • Spectral Resolution 25 mÅ
  • The Broad Band Filter Imager images the
    photosphere and chromosphere in six bands between
    380 670 nm at the highest resolution thus far
    of 0.053 arcsec pixels
  • The Narrow Band Filter Imager measures vector
    magnetic fields and Dopplergrams using a tunable
    filter
  • Spectral Coverage 5170 6570 Å
  • Magnetic Sensitivity 5 G (long) 50 G (trans)
  • Doppler Velocities 50 100 m/s

13
How good is the pointing and image stability?
  • The telescope is pointed using a sun sensor and
    the spacecraft provided attitude control system.
  • Due to orbital variation and jitter, the pointing
    stability ranges from 0.7 arcsec/sec to 5 arcsec
    per hour.
  • To recover the diffraction limited performance
    for the OTA, a correlation tracker controls a
    tip-tilt mirror located in the collimated beam
    exiting the OTA. The combination improves the
    expected image stability for the OTA/FPP to
    0.06 arcsec/10 sec and 2 arcsec per hour.

14
EUV Imaging Spectrometer
  • The EIS is a joint effort between MSSL and NRL.
  • EIS provides temperature and density diagnostics
    of coronal and transition region plasmas and will
    attempt to detect reconnection flows.
  • Properties
  • Wavelengths 170-210 Å, 250-290 Å
  • Resolution Spatial 1.0 arcsec pixel Spectral
    2.23 mÅ/pixel
  • Slits1 x 512 and 2 x 512 arcsec2
  • Slot 40 x 512 and 250 x 512 arcsec2

EIS final preparations
15
The X-Ray Telescope
  • XRT Properties
  • Optics - Wolter I Grazing Incidence Telescope
  • Focal Length 2700 cm
  • Geometric Area 5 cm2
  • Shutter/Analysis Filters
  • texp 1ms to 16s
  • 9 X-ray, 1 G-band filter
  • 1-30 MK temperature response range
  • Camera
  • 2048x2048 CCD
  • 1 arcsec pixels

The XRT is a collaborative effort between SAO
(mirror, filters, structure, mechanical systems)
and ISAS (camera sensor and electronics).
Mounting the XRT to the spacecraft
XRT Diameter 0.42 m Mass 48.4 kg
16
XRT Grazing Incidence Light Path
17
Filter Wheels
18
Temperature Response
19
XRT Science Goals
  • Coronal Mass Ejections
  • Coronal Heating
  • Reconnection and Jets
  • Flare Energetics
  • Photospheric-Coronal Coupling

20
XRT Observation Modes
  • Dynamics
  • Rapid evolution associated with reconnection and
    plasma instabilities
  • High Cadence
  • Energetics
  • The thermal evolution of structures heating
    cooling
  • The emission measure evolution of structures up
    flows down flows
  • Multiple filters
  • Topology
  • Identify the magnetic connections that control
    the heating and dynamics
  • Large FOV, long and short exposures

21
XRT First Light
28 October 2006
Hinode XRT Quiet Sun
22
28 October 2006
Hinode XRT False Color
23
?????X???????????
5 arcmin 220,000km)
30 arcsec 22,000km)
30 arcsec 22,000km)
24
SXT and XRT comparison
Trish Jibben
25
Al-Poly Filter
Al-Poly
Trish Jibben
26
C-Poly Filter
C-Poly
Trish Jibben
27
Be-Thin Filter
thin-Be
Trish Jibben
28
XRT Shows Extent of Structure Surrounding ARs
29
A typical corona (QS small AR) requires gt104
dynamic range
Combined 4s 0.5s XRT exposures, Thin Al filter.
30
Fine details in active regions
1 arcmin
31
B vs. X
MDI Magnetogram
XRT Thin Ti, 1 sec., 11/04/06
32
Photosphere-corona observations with SOT
XRT v. SOT G-band 14 November 2006 Magnetic Field
bifurcation over light bridge
Jonathan Cirtain
33
Detailed Views of AR from XRT
Small AR near CMP
Thin Al/Poly 1 sec
Jonathan Cirtain
34
Cavity structures seen at limb
Trish Jibben
35
Synoptic Sun-Center program
Trish Jibben
36
TRACE and XRT are complimentary
TRACE 11/13/06
XRT 11/13/06
Leon Golub
37
AR 10930 in X-1.5 Flare (Be-Thin)
Monica Bobra
38
Downflows seen in active region
David McKenzie
Note highly sheared inner and unsheared outer
loops in flaring region.
39
EIS view of shrinking loops at limb
David H. Brooks
40
EIS Slit Raster Movie
David H. Brooks
I
Distance
41
TRACE shrinking loops movie
Kathy Reeves
42
Combined SOT - XRT Observations
Joten Okamoto
43
Polar Jets - Numerous Events
Trish Jibben
44
Polar Jets - Theory
Shimojo, M., and Shibata, K., ApJ 542, 1100 (2000)
From the Hudson Solar Cartoon Archive
(http//solarmuri.ssl.berkeley.edu/hhudson/cartoo
ns/overview.html)
45
Total Solar Eclipse - 19 March 2007
Kano Ryouhei - XRT CO
46
Transit of Mercury Mosaic 8 November 2006
47
On-orbit measurement of PRFM. Weber and XRT Team
XRT Al_poly/Open 08-Nov-06 235031 16.39s
512x5121 pixel 1 arcsecondMercury traversed
the FOV horizontally about 1 arcsec during this
16.4 sec exposure. Mercurys angular diameter
10 arcsec.Analysis of three columns of pixels
perpendicular to planetary velocity.
Surface plot of intensity inside the subregion
box.Mercurys shadow has an obvious effect.Edge
blurring along the direction of velocity is
minimal, but we analyzed three columns in the
perpendicular direction anyway.
48
On-orbit measurement of PRF(M. Weber and XRT
Team)
Light-curves along 3 central columns through
shadow.The mean of these curves is analyzed on
the right (Northern) edge. We varied the sigma
of a 2D Gaussian convolved with a 2D circular
step-function shadow to fit the drop-off.
Intensity
Arcseconds (along Y-axis)
Dashed line mean of three columns in previous
plot.Diamonds data points used for fitting the
model.Error bars on data deviation of data
about mean (probably a bit generous).Solid line
best model fitBest fit Gaussian sigma of 0.6
/- 0.07 arcsec.FWHM 1.0 /- 0.12 arcsec
Mean Intensity
Arcseconds (along Y-axis)
49
Downloading XRT and SOT Data
  • Virtual Solar Observatory
  • http//sdac.virtualsolar.org/cgi-bin/search
  • Lockheed Martin Data Repository
  • http//sot.lmsal.com/sot-data
  • Hinode XRT Observing Proposals
  • http//solar.physics.montana.edu/HINODE/XRT
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