Fullsun temperature distribution and classification of coronal structures

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Full-sun temperature distribution and
classification of coronal structures

• N. Narukage (ISAS/JAXA)
• M. Shimojo, T. Sakao, R. Kano,K. Shibasaki, E.
  E. DeLuca, M. A. Weber,S. H. Saar, P. R. Jibben,
  S. Tsuneta, and Japan-US XRT Team

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Outline

• XRT filters
• Coronal temperature diagnostics using filter
  ratio method
• Full Sun temperature map
• EM-T diagram
• Summary

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1. XRT 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
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1. XRT filters
XRT makes us possible to derive coronal
temperature of lt 2MK.
This figure shows temperature responses of each
X-ray analysis filter. note You can overlap each
X-ray analysis filter of FW1 and FW2.
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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
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2. filter ratio method

• Filter ratio method

Assumption XRT observe same plasma with filter1
and filter2.
CAVEAT The derived temperature with filter ratio
method is the mean temperature biased by filters.
ratio of temperature response
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2. filter ratio method
2007/02/22 0002 filter Al-mesh and Ti-poly,
Max binning 4x4 Te error lt 20, photon noise lt
20
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3. Full Sun temperature map
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3. Full Sun temperature map

• using data of synoptic observation (4 data sets a
  day)
• Open / thin Al mesh - long exp.
• Open / thin Al mesh - short exp.
• Open / Ti poly - long exp.
• Open / Ti poly - short exp.
• Dark
• thin Al mash Ti poly pair
• Temperature is deriveduniquely at a wide range
  of 0.5MK10MK.
• Especially, this pair is sensitive to 1MK3MK
  plasma.
• This pair is suitable to make full Sun
  temperature map.

We dont consider the effect of scattered light
and mesh pattern of Al mesh filter.
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3. Full Sun temperature map
2007/02/22 0002 filter Al-mesh and Ti-poly,
Max binning 4x4 Te error lt 20, photon noise lt
20
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4. EM-T diagram
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4. EM-T diagram
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4. EM-T diagram
T lt 2MK Yohkoh/SXTcould not observe theplasma
in thistemperatureregion.
Where the data points on this diagram are located
on the solar disk?
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4. EM-T diagram
Coronal Hole
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4. EM-T diagram
Quiet Region
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4. EM-T diagram
cool plasma from AR
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4. EM-T diagram
cool flow from AR
Sakao et al. 2007
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4. EM-T diagram
foot point of AR loop
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4. EM-T diagram
around AR XBP
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4. EM-T diagram
This region is a new view by XRT, hot (as AR) but
low density (as QR).
long loop from AR
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EIT 171 A did not detect the long loop from
active region.
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long loop from AR
Hinode XRT
Yohkoh SXT
Yohkoh/SXT could not resolve this feature
sufficiently.
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4. EM-T diagram
Active Region
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4. EM-T diagram

• Active Region
• Long loop from AR
• around AR XBP
• foot point of AR loop
• Quiet Region
• cool flow from AR
• Coronal Hole

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4. EM-T diagram
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4. EM-T diagram
Rosner-Tucker-Vaiana scaling law
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4. EM-T diagram
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5. Summary

• XRT makes us possible to derive the coronal
  temperature in not only active region (1x1) but
  also quiet sun and coronal hole (4x4).
• Using the EM-T diagram, coronal structure is
  nicely classified.
• The length of loop and heating flux determine the
  coronal structure.
• Future workexamine the relation between heating
  flux and B for the clue to solving the big
  coronal heating question.

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END

• Thank you very much
• for your attention.

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4. EM-T diagram