Evolution of black hole low-mass binaries

Details Evolution of black hole low-mass binaries Evolution of black hole low-mass binaries

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...338...69e&link_type=abstract

Astronomy and Astrophysics, v.338, p.69-74 (1998)

Physics

10

Stars: Evolution, Black Hole Physics, X-Rays: Stars

Scientific paper

Several evolutionary sequences with low mass secondaries as donors and black holes as accretors are calculated. Adopting a simple estimate for the efficiency of magnetic braking we have determined the bifurcation period Pbif, separating converging from diverging binary systems, to be ~ 1 day. It is shown that in converging binary systems, similar to neutron star binaries with low-mass secondaries, evolution proceeds towards very short orbital periods with continous accretion or it ends by formation of system with a low mass helium white dwarf and a black hole. If the final orbital period of the latter system is less than 10 hours, it is possible that the system will reappear as a persistent X-ray source with ultra-short orbital period. For systems which evolve towards very short orbital periods there always is a phase in which the mass accretion rate exceeds a certain dot {M}crit(irr) above which the system is a persistent X-ray source. By comparing evolutionary sequences for different black hole masses it is shown that for a more massive black hole as accretor the range in which mass transfer is unstable is larger than for a less massive black hole. It is shown that after the common envelope (CE) phase, during the extensive high-velocity wind stage (before the collapse to a black hole) only helium stars of rather low mass end up with orbital periods lower than Pbif which enables them to evolve towards the short orbital period range where the majority of the low-mass X-ray binaries ( LMXB) with black holes as accretors are observed. This implies that the pre-CE progenitors of black holes in these systems had masses <= 25 Msun

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