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Flare Plasma Iron AbundanceThe 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 >approx.10 MK 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.
Document ID
20080030286
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Dennis, Brian R.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Dan, Chau
(Oklahoma Univ. Norman, OK, United States)
Jain, Rajmal
(Physical Research Lab. Ahmedabad, India)
Schwartz, Richard A.
(Catholic Univ. of America Greenbelt, MD, United States)
Tolbert, Anne K.
(Wyle Information Systems Greenbelt, MD, United States)
Date Acquired
August 24, 2013
Publication Date
May 26, 2008
Subject Category
Plasma Physics
Meeting Information
Meeting: AGU meeting for the special session of the Solar Physics Division of the American Astronomical Society
Location: Fort Lauderdale, FL
Country: United States
Start Date: May 26, 2008
End Date: May 31, 2008
Distribution Limits
Public
Copyright
Other

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