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The Solar Photospheric-to-Coronal Fe abundance from X-ray Fluorescence Lines View all abstracts by submitter

Kenneth Phillips   Submitted: 2012-01-03 05:44

The ratio of the Fe abundance in the photosphere to that in coronal flare plasmas is determined by X-ray lines within the complex at 6.7 keV (1.9~AA) emitted during flares. The line complex includes the He-like Fe (fexxv) resonance line w (6.70 keV) and Fe K α lines (6.39, 6.40 keV), the latter being primarily formed by the fluorescence of photospheric material by X-rays from the hot flare plasma. The ratio of the Fe K α lines to the fexxv w depends on the ratio of the photospheric-to-flare Fe abundance, heliocentric angle heta of the flare, and the temperature Te of the flaring plasma. Using high-resolution spectra from X-ray spectrometers on the {em P78-1} and {em Solar Maximum Mission} spacecraft, the Fe abundance in flares is estimated to be 1.6pm 0.5 and 2.0 pm 0.3 times the photospheric Fe abundance, the {em P78-1} value being preferred as it is more directly determined. This enhancement is consistent with results from X-ray spectra from the {em RHESSI} spacecraft, but is significantly less than a factor 4 as in previous work.

Authors: K. J. H. Phillips
Projects: Yohkoh-BCS

Publication Status: Accepted by MNRAS
Last Modified: 2012-01-03 08:25
Go to main E-Print page  Wave-particle interactions in non-uniform plasma and the interpretation of Hard X-ray spectra in solar flares  Heating of Flare Loops With Observationally Constrained Heating Functions  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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