Energy-height relation for hard X-ray footpoint sources observed by RHESSI.

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Energy-height relation for hard X-ray footpoint
sources observed by RHESSI.

• TOMASZ MROZEK
• ASTRONOMICAL INSTITUTE, WROCLAW UNIVERSITY

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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
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.
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Inverse it
From thick-target model ( )
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Brown, J. C., Aschwanden, M. J., and Kontar, E.
P., 2002, Solar Phys. 210, 373
Aschwanden, M. J., Brown, J. C., and Kontar, E.
P., 2002, Solar Phys. 210, 383
C7.5 N16W80 NOAA 9825
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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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Number of events
Number of events
Number of events
Thick of the collisional-stopping region km
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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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THE END...?