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The evolution of primary stars (30–40 \(\mathrm M_{\odot }\)) in massive close binary systems

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Abstract

We present evolutionary models of primary stars with initial masses in the range of 30 to 40 \(\mathrm M_{\odot }\), evolving in massive binary systems, possible progenitors of gravitational wave sources. The binary systems have an initial mass ratio of 0.9, an initial orbital period of 3 days and an accretion efficiency of 10%. The evolution of the primary stars in those systems is followed from the main sequence to the formation of the carbon-oxygen core. In addition, the evolution of two primaries with the lowest initial masses is calculated to the iron core formation. The masses of the helium and carbon-oxygen cores formed in primary stars are compared with the masses of cores formed in single stars with the same initial masses. The initial mass limit for the black hole formation for this selected type of massive binaries is established between 32 and 34 \(\mathrm M_{\odot }\). All models are calculated with the MESA (Modules for Experiments in Stellar Astrophysics) numerical code.

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Data Availability Statement

This manuscript has no associated data or the data will not be deposited. [Authors’ comment: The datasets generated during and/or analysed during the current study are available from the corresponding author on reasonable request and at Zenodo.org.]

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Acknowledgements

During the work on this paper the authors were financially supported by the Ministry of Education and Science of the Republic of Serbia through the contract 451-03-9/2021-14/200002.

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  1. Astronomical Observatory, Volgina 7, Belgrade, Serbia

    Jelena Petrovic

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  1. Jelena Petrovic
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All the authors were involved in the preparation of the manuscript. All the authors have read and approved the final manuscript.

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Correspondence to Jelena Petrovic.

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Petrovic, J. The evolution of primary stars (30–40 \(\mathrm M_{\odot }\)) in massive close binary systems. Eur. Phys. J. D 75, 162 (2021). https://doi.org/10.1140/epjd/s10053-021-00166-9

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