Iron Abundance of Flare Plasma

Details Iron Abundance of Flare Plasma Iron Abundance of Flare Plasma

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp44a..04d&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP44A-04

Other

7509 Corona, 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos

Scientific paper

The equivalent width of the iron-line complex at 6.7 keV seen in flare X-ray spectra suggests that the iron abundance of the hottest plasma at temperatures >~10MK may sometimes be significantly lower than the nominal coronal abundance of four times the photospheric value that is commonly assumed. This conclusion is based on X-ray spectral observations of several flares seen in common with the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Solar X-ray Spectrometer (SOXS) on the second Indian geostationary satellite, GSAT-2. The implications of this will be discussed as it relates to the origin of the hot flare plasma - either plasma already in the corona that is directly heated during the flare energy release process or chromospheric plasma that is heated by flare-accelerated particles and driven up into the corona. Other possible explanations of lower-than-expected equivalent widths of the iron-line complex will also be discussed.

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