Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9307d&link_type=abstract
American Astronomical Society Meeting 210, #93.07; Bulletin of the American Astronomical Society, Vol. 39, p.212
Other
Scientific paper
RHESSI X-ray spectroscopy is possible down to the lowest energies ( 3 to 6 keV depending on attenuator state) provided that the many instrumental effects are adequately accounted for. Fully exploiting these observations, especially at the lower end of the RHESSI spectral range below 20 keV, has proven to be challenging given the complexity of the instrument response and the many effects that must be considered in determining the incident photon spectrum from the measured count-rate spectrum. These effects include the strong attenuation of the material overlying the detectors, the instrument background lines from the germanium detectors and the tungsten grids, the K-escape process and other mechanisms that result in lower than expected pulse amplitudes, electronic effects at high count rates such as pulse pile-up and change in gain, detector-to-detector differences, variations in the non-flare background spectrum, etc. We will discuss the current status of our ability to estimate the magnitude of all of these effects and to determine the properties of the incident photon spectrum using the forward-fitting method. The introduction of Chianti version 5.2 has allowed us to fit expected thermal continuum and line spectra with a single temperature or a given distribution of temperatures and to determine the iron abundance from the intensity of the iron-line complex peaking at 6.7 keV. Pulse pile-up and albedo corrections can now be applied during the spectral fitting process allowing us to determine best-fit estimates of both the thermal and nonthermal components of the photon spectrum coming directly from the X-ray source(s). While the separation of the thermal and nonthermal components remains difficult, utilizing the new ability to reliably measure the photon spectrum below 10 keV combined with the temporal and spatial signatures make it possible to resolve this issue in specific cases with greater reliability than has previously been possible.
Dang Leeann
Dennis Brian R.
Schwartz Russell
Tolbert Kimberley A.
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