Computer Science – Sound
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5908a&link_type=abstract
American Astronomical Society, AAS Meeting #211, #59.08; Bulletin of the American Astronomical Society, Vol. 39, p.842
Computer Science
Sound
Scientific paper
The recent recommended large reduction in the solar oxygen abundance--mainly motivated by spectral synthesis of a weak forbidden O I absorption (6300 A) using 3D convection models---has provoked consternation in the helioseismology community: the spectacular agreement between measured interior sound speed profiles and predictions based on the historical abundance (850 ppm relative to hydrogen) completely unravels at the new lower value (450 ppm). At the same time, molecular tracers of the oxygen abundance, such as CO, indicate a value closer to 700 ppm, when the photospheric temperatures in the region of peak molecular concentration are carefully adjusted to match the temperature sensitive wings of the Ca II H and K lines. (One does derive 450 ppm when the unaltered 3D models are used, but these simulations are too cool in the upper photosphere where the molecular diagnostics arise.) In order to reconcile these disparate results, I have reconsidered the formation of the [O I] 6300 feature using an alternative 3D convection model that matches key observational constraints such as the visible continuum center-limb behavior, and calibrated continuum intensities at disk center. As compared with the previous work of Allende Prieto, Asplund, and collaborators, I find that the so-called "1D-to-3D abundance correction" not only is very small, contrary to their study, but also goes in the opposite direction. The consequence is an oxygen abundance of about 650 ppm from 3D [O I]: not too high, not too low, but just right (in the middle). This work was supported by NSF. I thank the CO5BOLD collaboration for making available snapshots from their 3D time dependent solar convection simulations.
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