0472116 - ASÚ 2017 RIV FR eng J - Článek v odborném periodiku
Kruckow, M.U. - Tauris, T.M. - Langer, N. - Szécsi, Dorottya - Marchant, P. - Podsiadlowski, Ph.
Common-envelope ejection in massive binary stars Implications for the progenitors of GW150914 and GW151226.
Astronomy & Astrophysics. Roč. 596, December (2016), A58/1-A58/13. ISSN 0004-6361. E-ISSN 1432-0746
Grant CEP: GA ČR(CZ) GA14-02385S
Institucionální podpora: RVO:67985815
Klíčová slova: stars * evolution * black holes
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 5.014, rok: 2016 ; AIS: 1.581, rok: 2016
DOI: https://doi.org/10.1051/0004-6361/201629420

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.
Trvalý link: http://hdl.handle.net/11104/0269461