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Common-envelope ejection in massive binary stars Implications for the progenitors of GW150914 and GW151226
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SYSNO ASEP 0472116 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Common-envelope ejection in massive binary stars Implications for the progenitors of GW150914 and GW151226 Author(s) Kruckow, M.U. (DE)
Tauris, T.M. (DE)
Langer, N. (DE)
Szécsi, Dorottya (ASU-R) ORCID
Marchant, P. (DE)
Podsiadlowski, Ph. (US)Source Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 596, December (2016), A58/1-A58/13Number of pages 13 s. Publication form Online - E Language eng - English Country FR - France Keywords stars ; evolution ; black holes Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA14-02385S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000390797900106 EID SCOPUS 85002935925 DOI https://doi.org/10.1051/0004-6361/201629420 Annotation We analyse the common-envelope (CE) stage of the traditional formation channel in binaries where the first-formed compact object undergoes an in-spiral inside the envelope of its evolved companion star and ejects the envelope in this process. Massive stars in a wide range of metallicities and with initial masses of up to at least 115 M-circle dot may shed their envelopes and survive CE evolution, depending on their initial orbital parameters, similarly to the situation for intermediate-and low-mass stars with degenerate cores. In addition to being dependent on stellar radius, the envelope binding energies and lambda-values also depend on the applied convective core-overshooting parameter, whereas these structure parameters are basically independent of metallicity for stars with initial masses below 60 M-circle dot. Metal-rich stars greater than or similar to 60 M-circle dot become luminous blue variables and do not evolve to reach the red giant stage. We conclude that based on stellar structure calculations, and in the view of the usual simple energy budget analysis, events like GW150914 and GW151226 might be produced by the CE channel. Calculations of post-CE orbital separations, however, and thus the estimated LIGO detection rates, remain highly uncertain. Workplace Astronomical Institute Contact Anežka Melichárková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2017
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