Case C mass transfer in the evolution of black hole binaries

Details Case C mass transfer in the evolution of black hole binaries Case C mass transfer in the evolution of black hole binaries

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13r.385l&link_type=abstract

In: Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 J

Astronomy and Astrophysics

Astronomy

Dense Stellar Systems

Scientific paper

Earlier works have shown that if the Fe core in a presupernova star is to be sufficiently massive to collapse into a black hole earlier in the evolution of the star the He core must be covered (clothed) by a hydrogen envelope during He core burning and removed only following this in e.g. common envelope evolution. This is classified as Case C mass transfer. In this work we argue for Case C mass transfer on the basis of binary evolution. The giant progenitor of the black hole will have a large radius about 1000 solar radius at the end of its supergiant stage. Its lifetime at that point will be short about 1000 yrs so it will not expand much further. Thus the initial giant radius for Case C mass transfer will be constrained to a narrow band about 1000 solar radius. This have the consequence that the final separation following common envelope evolution will depend nearly linearly on the mass of the companion which becomes the donor after the He core of the giant has collapsed into the black hole. We show that the reconstructed preexplosion separation of the black hole binaries fit well the linear relationship.

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