RHESSI Line and Continuum Observations of Super-hot Flare Plasma

We use RHESSI high-resolution imaging and spectroscopy observations from ~5 to 100 keV to characterize the hot thermal plasma during the 2002 July 23 X4.8 flare. These measurements of the steeply falling thermal X-ray continuum are well fit throughout the flare by two distinct isothermal components:...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2010-12, Vol.725 (2), p.L161-L166
Main Authors: Caspi, A, Lin, R. P
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ELECTROMAGNETIC RADIATION
EMISSION
EVOLUTION
GAMMA RADIATION
HOT PLASMA
IONIZING RADIATIONS
MAIN SEQUENCE STARS
PLASMA
RADIATIONS
SOLAR ACTIVITY
SOLAR FLARES
SPECTROSCOPY
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR FLARES
SUN
X RADIATION
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Summary:We use RHESSI high-resolution imaging and spectroscopy observations from ~5 to 100 keV to characterize the hot thermal plasma during the 2002 July 23 X4.8 flare. These measurements of the steeply falling thermal X-ray continuum are well fit throughout the flare by two distinct isothermal components: a super-hot (Te > 30 MK) component that peaks at ~44 MK and a lower-altitude hot (Te 25 MK) component whose temperature and emission measure closely track those derived from GOES measurements. The two components appear to be spatially distinct, and their evolution suggests that the super-hot plasma originates in the corona, while the GOES plasma results from chromospheric evaporation. Throughout the flare, the measured fluxes and ratio of the Fe and Fe-Ni excitation line complexes at ~6.7 and ~8 keV show a close dependence on the super-hot continuum temperature. During the pre-impulsive phase, when the coronal thermal and non-thermal continua overlap both spectrally and spatially, we use this relationship to obtain limits on the thermal and non-thermal emission.
ISSN:2041-8205
2041-8213
DOI:10.1088/2041-8205/725/2/L161