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
Energy-height relation for hard X-ray footpoint sources observed
by RHESSI.
TOMASZ MROZEK
ASTRONOMICAL INSTITUTE, WROCŁAW UNIVERSITY
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
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
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
3. RESULTS
• 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.
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.
Num
ber
of
events
Num
ber
of
events
Thick of the collisional-stopping region [km]
Num
ber
of
events
Comparision between several models of density (Aschwanden et al. 2002) and densities obtained from RHESSI observations.
4. QUESTIONS
4. QUESTIONS
THE END...?