energy-height relation for hard x-ray footpoint sources observed by rhessi
DESCRIPTION
TOMASZ MROZEK ASTRONOMICAL INSTITUTE, WROCŁAW UNIVERSITY. Energy-height relation for hard X-ray footpoint sources observed by RHESSI. 2. METHOD. - Make images in the wide energy range divided into intervals of few keV , in steps of 1 keV . - Determine positions - PowerPoint PPT PresentationTRANSCRIPT
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Energy-height relation for hard X-ray footpoint sources observed
by RHESSI.
TOMASZ MROZEK
ASTRONOMICAL INSTITUTE, WROCŁAW UNIVERSITY
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The altitude of centroids (asterixs) above a reference level versus the energy of hard X-
rays. The power-law function fit is presented with dotted line.
2. METHOD
- Make images in the wide energy range divided into intervals of few keV, in steps of 1 keV.
- Determine positions of centroids
- Fit the power-law function:
a
keVzz
20)( 0
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Inverse it:
a
z
zz
1
0
20)(
3
00
12 11105.1)(
cm
z
z
z
Mm
azn
b
12
a
b
dz
d
Kdz
zdNzn
)()(
From thick-target model ( ):E
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Aschwanden, M. J., Brown, J. C., and Kontar, E. P., 2002, Solar Phys. 210, 383
* C7.5
* N16W80
* NOAA 9825
Brown, J. C., Aschwanden, M. J., and Kontar, E. P., 2002, Solar Phys. 210, 373
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3. RESULTS
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• PseudoColor picture– the TRACE 171 Å image, obtained after the maximum; • contours – the TRACE 171 Å images obtained during the impulsive phase, the times
are given above each frame; • crosses – locations of centroids of hard X-ray sources, the times are the same as
above, brighter colours represent the higher energies; the solar limb is overplotted.
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Relations made for consecutive 12s intervals covering the first, main peak.Time evolution is represented by the brightness. The first interval is the darkest one.
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Num
ber
of
events
Num
ber
of
events
Thick of the collisional-stopping region [km]
Num
ber
of
events
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Comparision between several models of density (Aschwanden et al. 2002) and densities obtained from RHESSI observations.
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4. QUESTIONS
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4. QUESTIONS
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THE END...?