Dark matter heat transport can erase convective cores in solar-mass stars, yielding asteroseismic constraints on dark matter-nucleon scattering and a 4 sigma hint of dark matter-electron scattering in KIC 8228742 that conflicts with direct detection limits.
A Reappraisal of the Solar Photospheric C/O Ratio
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abstract
Accurate determination of photospheric solar abundances requires detailed modeling of the solar granulation and accounting for departures from local thermodynamical equilibrium (LTE). We argue that the forbidden C I line at 8727 A is largely immune to departures from LTE, and can be realistically modeled using LTE radiative transfer in a time-dependent three-dimensional simulation of solar surface convection. We analyze the [C I] line in the solar flux spectrum to derive the abundance log epsilon(C)= 8.39 +/- 0.04 dex. Combining this result with our parallel analysis of the [O I] 6300 A line, we find C/O=0.50 +/- 0.07, in agreement with the ratios measured in the solar corona from gamma-ray spectroscopy and solar energetic particles.
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Asteroseismological constraints on--and hints of--dark matter interactions
Dark matter heat transport can erase convective cores in solar-mass stars, yielding asteroseismic constraints on dark matter-nucleon scattering and a 4 sigma hint of dark matter-electron scattering in KIC 8228742 that conflicts with direct detection limits.