Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.
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Asteroseismic structure inversions can be performed in acoustic and buoyancy coordinates, overcoming breakdowns for non-solar stars and removing the need for prior mass and radius knowledge in p-mode cases.
1D models show convective boundary mixing dominates the asteroseismic imprint of accretion in massive stars, robust to semiconvection changes but drastically altered without it, with thermal relaxation as key.
Detection of GW Vir-type g-mode pulsations in Kn 61 central star gives period spacing 21.526 s and asteroseismic mass 0.551 solar masses consistent with evolutionary tracks.
Interstellar objects may contribute enough baryonic mass to reduce the local dark matter halo density to 0.24 GeV/cm³.
Asteroseismic fits to g-dominated mixed modes in four red giants suggest convective overshooting rises with mass and yield a core rotation rate of 0.7409 μHz for KIC 11968334.
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Unveiling the nature of barium stars. I. Asteroseismic masses and the evolutionary link between Ba dwarfs and giants
Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.