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Abstract: We use very precise frequencies of low-degree solar-oscillation modesmeasured from 4752 days of data collected by the Birmingham Solar-OscillationsNetwork (BiSON) to derive seismic information on the solar core. We comparethese observations to results from a large Monte Carlo simulation of standardsolar models, and use the results to constrain the mean molecular weight of thesolar core, and the metallicity of the solar convection zone. We find that onlya high value of solar metallicity is consistent with the seismic observations.We can determine the mean molecular weight of the solar core to a very highprecision, and, dependent on the sequence of Monte Carlo models used, find thatthe average mean molecular weight in the inner 20% by radius of the Sun rangesfrom 0.7209 to 0.7231, with uncertainties of less than 0.5% on each value. Ourlowest seismic estimate of solar metallicity is Z=0.0187 and our highest isZ=0.0239, with uncertainties in the range of 12-19%. Our results indicate thatthe discrepancies between solar models constructed with low metallicity and thehelioseismic observations extend to the solar core and thus cannot beattributed to deficiencies in the modeling of the solar convection zone.



Author: William J. Chaplin, Aldo M. Serenelli, Sarbani Basu, Yvonne Elsworth, Roger New, Graham A. Verner

Source: https://arxiv.org/







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