The Solar Flare Iron Abundance

Abstract

The abundance of iron is measured from emission line complexes at 6.65 keV (Fe line) and 8 keV (Fe/Ni line) in {\em RHESSI} X-ray spectra during solar flares. Spectra during long-duration flares with steady declines were selected, with an isothermal assumption and improved data analysis methods over previous work. Two spectral fitting models give comparable results, viz. an iron abundance that is lower than previous coronal values but higher than photospheric values. In the preferred method, the estimated Fe abundance is $A(\mathrm{Fe})=7.91\pm 0.10$ (on a logarithmic scale, with $A(\mathrm{H})=12$), or $2.6\pm 0.6$ times the photospheric Fe abundance. Our estimate is based on a detailed analysis of 1,898 spectra taken during 20 flares. No variation from flare to flare is indicated. This argues for a fractionation mechanism similar to quiet-Sun plasma. The new value of $A(\mathrm{Fe})$ has important implications for radiation loss curves, which are estimated.

Accepted by Astrophysical Journal

References in corpus (2)

• Highly Efficient Modeling of Dynamic Coronal Loops
• Highly ionized Fe X-ray lines at energies 7.7-8.6 keV

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