Using Gamma-Ray Line Observations to Determine the Chromospheric Neon/Oxygen Abundance Ratio

Details Using Gamma-Ray Line Observations to Determine the Chromospheric Neon/Oxygen Abundance Ratio Using Gamma-Ray Line Observations to Determine the Chromospheric Neon/Oxygen Abundance Ratio

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1910s&link_type=abstract

American Astronomical Society, SPD meeting #40, #19.10; Bulletin of the American Astronomical Society, Vol. 41, p.848

Astronomy and Astrophysics

Astronomy

Scientific paper

There has been a lively debate concerning the solar neon abundance since Asplund et al. (2005) reported a significant downward revision of C, N, and O abundances from those compiled by Grevesse and Sauval (1998). This lower metallicity has affected solar opacity to the extent that solar interior models are no longer consistent with helioseismology data. As Ne is not measured directly in the photosphere, Bahcall et al. (2005) have suggested that a solar Ne abundance a factor of 3 higher than the adopted value (Ne/O 0.15) could resolve this discrepancy. A factor of this magnitude appears to be inconsistent with quiet-Sun transition-region measurements (Young 2005) and flaring-coronal observations (Schmeltz et al. 2005; Landi et al. 2007). However, there are concerns whether these abundances measured in the upper solar atmosphere reflect the situation in the photosphere. We have fit solar flare gamma-ray line spectra using newly developed theoretical models of nuclear emission from proton and alpha-particle interactions deep in the chromosphere to determine the Ne/O abundance. We report on our measurements of this ratio in flares observed by the Solar Maximum Mission spectrometer.

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