HR: 09:00h
AN: SH31A-03    [Abstracts]
TI: RHESSI soft X-ray imaging spectroscopy of a flare
AU: * Hudson, H
EM: hhudson@ssl.berkeley.edu
AF: SSL/UCB, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Caspi, A
EM: cepheid@ssl.berkeley.edu
AF: SSL/UCB, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Dennis, B
EM: Brian.r.dennis@nasa.gov
AF: NASA-GSFC, Laboratory for Astron. & Solar Phys., Greenbelt, MD 21770 United States
AU: Phillips, K
EM: phillips@stars.gsfc.nasa.gov
AF: NASA-GSFC, Laboratory for Astron. & Solar Phys., Greenbelt, MD 21770 United States
AB: We apply RHESSI imaging spectroscopy to a well-observed solar flare on 26~April~2003. This GOES M2-class flare (N20W69) exercised all three of the RHESSI shutter states, and was simultaneously observed by the RESIK high-resolution X-ray spectrometer on board the CORONAS-F spacecraft (Dennis et al., 2005). It thus provides an excellent opportunity to study the behavior of the high-throughput RHESSI observations of the Fe~emission-line complex at ~6.7~keV. The equivalent width of this feature has a unique dependence on the assumed isothermal temperature of the source (Phillips, 2004). Comparing this feature-derived temperature between the onset and decay phases of the event, we note a discrepancy between it and the temperature derived directly from the continuum. We analyze the causes of this discrepancy in terms of image morphology, non-isothermality, non-equilibrium excitation, and instrument properties.
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
DE: 7594 Instruments and techniques
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly