The evolution of black hole mass and angular momentum

We show that neither accretion nor angular momentum extraction is likely to lead to significant changes in the mass M1 or angular momentum parameter a* of a black hole in a binary system with realistic parameters. Current values of M1 and a* therefore probably reflect those at formation. We show further that sufficiently energetic jet ejection powered by the rotational energy of a black hole can stabilize mass transfer in systems with large adverse mass ratios, and even reduce the mass transfer rate to the point where the binary becomes transient.

[1]  Wei Cui,et al.  To appear in The Astrophysical Journal Letters BLACK HOLE SPIN IN X-RAY BINARIES: OBSERVATIONAL CONSEQUENCES II , 1997 .

[2]  Ulrich Kolb.  Soft X-ray transients in the Hertzsprung gap , 1998 .

[3]  Jochen Greiner,et al.  RXTE Observations of QPOs in the Black Hole Candidate GRS 1915+105 , 1997 .

[4]  G. J. Savonije,et al.  Evolutionary status of bright, low-mass x-ray sources¹ , 1983 .

[5]  K. Thorne.  Disk-Accretion onto a Black Hole. II. Evolution of the Hole , 1974 .

[6]  D. Christodoulou,et al.  Reversible transformations of a charged black hole , 1971 .

[7]  J. Bardeen,et al.  Kerr Metric Black Holes , 1970, Nature.

[8]  Ewa Szuszkiewicz,et al.  Why Low-Mass Black Hole Binaries Are Transient , 1997 .

[9]  G. J. Savonije,et al.  Evolutionary status of bright, low-mass x-ray sources/sup 1/ , 1983 .

[10]  R. Blandford,et al.  Electromagnetic extraction of energy from Kerr black holes , 1977 .

[11]  C. Sarazin,et al.  High-mass X-ray binary populations. 1: Galactic modeling , 1995 .

[12]  Hydrodynamical Studies of Wind Accretion onto Compact Objects: Two-dimensional Calculations , 1996, astro-ph/9610245.

[13]  W. Cui,et al.  EVIDENCE FOR FRAME-DRAGGING AROUND SPINNING BLACK HOLES IN X-RAY BINARIES , 1997, astro-ph/9710352.

[14]  R. M. Hjellming,et al.  Episodic ejection of relativistic jets by the X-ray transient GRO J1655 - 40 , 1995, Nature.

[15]  P. Eggleton.  Approximations to the radii of Roche lobes , 1983 .

[16]  T. Zwitter,et al.  SS433: a black hole candidate? , 1989 .

[17]  B. Elmegreen,et al.  The largest molecular cloud complexes in the first galactic quadrant , 1986 .

[18]  Denis J. Evans,et al.  Recent developments in non-Newtonian molecular dynamics , 1998 .

[19]  J. Orosz,et al.  Optical Observations of GRO J1655–40 in Quiescence. I. A Precise Mass for the Black Hole Primary , 1996, astro-ph/9610211.

[20]  J. van Paradijs,et al.  On the Accretion Instability in Soft X-Ray Transients , 1996 .

[21]  G. Ghisellini,et al.  The bulk kinetic power of the jets of GRS 1915+105 , 1998, astro-ph/9810029.

[22]  D. Bhattacharya,et al.  Formation and evolution of binary and millisecond radio pulsars , 1991 .

[23]  Tom Oosterloo,et al.  Evidence that the compact object in SS433 is a neutron star and not a black hole , 1991, Nature.

[24]  D. Christodoulou.  Reversible and Irreversible Transformations in Black-Hole Physics , 1970 .

[25]  E. Regős,et al.  The Unusual Evolutionary State of GRO J1655 – 40 , 1998 .

[26]  Luciano Burderi,et al.  Black Hole Binaries and X-Ray Transients , 1996 .

[27]  Christopher A. Tout,et al.  Rapid binary star evolution for N-body simulations and population synthesis , 1997 .