Hidden Population of Algols

Malkov, O. Yu.; Kovaleva, D. A.; Yungelson, L. R.; Avvakumova, E. A.; Chulkov, Dmitry; Dluzhnevskaya, O. B.; Kniazev, A. Y.

doi:10.1515/astro-2017-0257

Cited by 2 publications

(1 citation statement)

References 14 publications

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“…Given their low mass these stars may be rejected by APOKASC or may be too dim to be seen in great numbers. Our prediction number of Algols is similar to the 0.1 − 0.2 per cent of Galactic disc stars predicted by Malkov et al (2017). Interaction is more likely in giant stars than in field dwarfs, which at least partly explains our greater predicted frequency.…”

Section: Binary Properties As a Function Of Mass And Orbital Periodsupporting

confidence: 87%

Binary stars in the Galactic thick disc

Izzard

Preece

Jofré

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The combination of asteroseismologically-measured masses with abundances from detailed analyses of stellar atmospheres challenges our fundamental knowledge of stars and our ability to model them. Ancient red-giant stars in the Galactic thick disc are proving to be most troublesome in this regard. They are older than 5 Gyr, a lifetime corresponding to an initial stellar mass of about 1.2 M . So why do the masses of a sizeable fraction of thick-disc stars exceed 1.3 M , with some as massive as 2.3 M ? We answer this question by considering duplicity in the thick-disc stellar population using a binary population-nucleosynthesis model. We examine how mass transfer and merging affect the stellar mass distribution and surface abundances of carbon and nitrogen. We show that a few per cent of thick-disc stars can interact in binary star systems and become more massive than 1.3 M . Of these stars, most are single because they are merged binaries. Some stars more massive than 1.3 M form in binaries by wind mass transfer. We compare our results to a sample of the APOKASC data set and find reasonable agreement except in the number of these thick-disc stars more massive than 1.3 M . This problem is resolved by the use of a logarithmically-flat orbital-period distribution and a large binary fraction.

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Section: Binary Properties As a Function Of Mass And Orbital Periodsupporting

confidence: 87%

Binary stars in the Galactic thick disc

Izzard

Preece

Jofré

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Semidetached double-lined eclipsing binaries: Stellar parameters and rare classes

Malkov

2019

Monthly Notices of the Royal Astronomical Society

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Semidetached eclipsing systems provide a unique opportunity to derive the basic properties of interacting binaries. The goal of this work is to collect and to make use of data on semidetached systems with available light and radial velocity curve solutions. I have compiled the most comprehensive list to date, of 119 semidetached double-lined eclipsing binaries, containing the orbital parameters and physical parameters of the components. I consider the classification of semidetached binaries and discuss gaps between various classes in the Hertzspung–Russell diagram. I list systems with component parameters that are inverted and briefly discuss their evolutionary state.

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Hidden Population of Algols

Cited by 2 publications

References 14 publications

Binary stars in the Galactic thick disc

Binary stars in the Galactic thick disc

Semidetached double-lined eclipsing binaries: Stellar parameters and rare classes

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