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2003MNRAS.341..385P - Mon. Not. R. Astron. Soc., 341, 385-404 (2003/May-2)
On the formation and evolution of black hole binaries.
PODSIADLOWSKI P., RAPPAPORT S. and HAN Z.
Abstract (from CDS):
We then present detailed binary evolution sequences for black hole binaries with secondaries of 2 to 17 M☉and demonstrate that in these systems the black hole can accrete appreciably even if accretion is Eddington-limited (up to 7 M☉for an initial black hole mass of 10 M☉) and that the black holes can be spun up significantly in the process. We discuss the implications of these calculations for well-studied black hole binaries (in particular GRS 1915+105) and ultraluminous X-ray sources of which GRS 1915+105 appears to represent a typical Galactic counterpart. We also present a detailed evolutionary model for Cygnus X-1, a massive black hole binary, which suggests that at present the system is most likely in a wind mass-transfer phase following an earlier Roche-lobe overflow phase. Finally, we discuss how some of the assumptions in the standard model could be relaxed to allow the formation of low-mass, short-period black hole binaries, which appear to be very abundant in nature.
Abstract Copyright: 2003 RAS
Journal keyword(s): black hole physics - gravitation - binaries: close - stars: individual: Cygnus X-1 - stars: individual: GRS 1915+105 - X-rays: stars
Simbad objects: 7
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