Statistics of Hot Plasmas in M/X Flares Using RHESSI Fe & Fe/Ni Line and Continuum Observations

Details Statistics of Hot Plasmas in M/X Flares Using RHESSI Fe & Fe/Ni Line and Continuum Observations Statistics of Hot Plasmas in M/X Flares Using RHESSI Fe & Fe/Ni Line and Continuum Observations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh41a0309c&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH41A-0309

Physics

7509 Corona, 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos, 7594 Instruments And Techniques, 7599 General Or Miscellaneous

Scientific paper

Observations by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) have shown that "super-hot" (T > ~30~MK) thermal plasmas are a somewhat common feature of (large) flares of GOES class M or X. However, the origins and evolution of such super-hot plasmas are still poorly understood. RHESSI observes solar photons >3 keV with a spectral resolution of ~1~keV FWHM, and is especially sensitive to flare plasmas hotter than ~10~MK. RHESSI's rich data set allows an unprecedented level of analysis of thermal flare plasma through imaging and spectroscopic observations of the thermal bremsstrahlung continuum and the Fe and Fe/Ni line complexes at ~6.7 and ~8~keV. Accurately characterizing the thermal plasma provides information about flare heating and cooling mechanisms and improves our understanding of flare energy transport and release. We present early results of a statistical survey of hot thermal plasmas in ~300 RHESSI-observed M/X-class flares (2002-2005), utilizing an analytical method to compare the thermal continuum and line emission (Caspi & Lin 2007). We present flare energetics, size, and temperature distributions and discuss the implications for the origins of super-hot thermal plasmas.

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