SMaSH+ survey data yields the first observationally grounded distributions of key parameters for 26 hierarchical massive triples, dominated by tight inner binaries and wider tertiaries with no strong mass-separation correlations.
The incidence of stellar mergers and mass gainers among massive stars
3 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Because the majority of massive stars are born as members of close binary systems, populations of massive main-sequence stars contain stellar mergers and products of binary mass transfer. We simulate populations of massive stars accounting for all major binary evolution effects based on the most recent binary parameter statistics and extensively evaluate the effect of model uncertainties. Assuming constant star formation, we find that $8^{+9}_{-4}\,\%$ of a sample of early type stars to be the product of a merger resulting from a close binary system. In total we find that $30^{+10}_{-15}\,\%$ of massive main-sequence stars are the product of binary interaction. We show that the commonly adapted approach to minimize the effects of binaries on an observed sample by excluding systems detected as binaries through radial velocity campaigns can be counterproductive. Systems with significant radial velocity variations are mostly pre-interaction systems. Excluding them substantially enhances the relative incidence of mergers and binary products in the non radial velocity variable sample. This poses a challenge for testing single stellar evolutionary models. It also raises the question of whether certain peculiar classes of stars, such as magnetic O-stars, are the result of binary interaction and it emphasizes the need to further study the effect of binarity on the diagnostics that are used to derive the fundamental properties (star-formation history, initial mass function, mass to light ratio) of stellar populations nearby and at high redshift.
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UNVERDICTED 3representative citing papers
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.
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
citing papers explorer
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Southern Massive Stars at High Angular Resolution (SMaSH+): Properties of hierarchical massive triples
SMaSH+ survey data yields the first observationally grounded distributions of key parameters for 26 hierarchical massive triples, dominated by tight inner binaries and wider tertiaries with no strong mass-separation correlations.
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The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors
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.
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Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.