Thermodynamics of binary black holes and neutron stars

Details Thermodynamics of binary black holes and neutron stars Thermodynamics of binary black holes and neutron stars

2001-08-28

arxiv.org/abs/gr-qc/0108070v2

Phys.Rev. D65 (2002) 064035; Erratum-ibid. D70 (2004) 129904

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

26 pages, revised version, modified appendix A, to appear in PRD

Scientific paper

10.1103/PhysRevD.65.064035

We consider compact binary systems, modeled in general relativity as vacuum or perfect-fluid spacetimes with a helical Killing vector k^\alpha, heuristically, the generator of time-translations in a corotating frame. Systems that are stationary in this sense are not asymptotically flat, but have asymptotic behavior corresponding to equal amounts of ingoing and outgoing radiation. For black-hole binaries, a rigidity theorem implies that the Killing vector lies along the horizon's generators, and from this one can deduce the zeroth law (constant surface gravity of the horizon). Remarkably, although the mass and angular momentum of such a system are not defined, there is an exact first law, relating the change in the asymptotic Noether charge to the changes in the vorticity, baryon mass, and entropy of the fluid, and in the area of black holes. Binary systems with M\Omega small have an approximate asymptopia in which one can write the first law in terms of the asymptotic mass and angular momentum. Asymptotic flatness is precise in two classes of solutions used to model binary systems: spacetimes satisfying the post-Newtonian equations, and solutions to a modified set of field equations that have a spatially conformally flat metric. (The spatial conformal flatness formalism with helical symmetry, however, is consistent with maximal slicing only if replaces the extrinsic curvature in the field equations by an artificially tracefree expression in terms of the shift vector.) For these spacetimes, nearby equilibria whose stars have the same vorticity obey the relation \delta M = \Omega \delta J, from which one can obtain a turning point criterion that governs the stability of orbits.

Affiliated with

Also associated with

No associations

Rating

Thermodynamics of binary black holes and neutron stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Thermodynamics of binary black holes and neutron stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Thermodynamics of binary black holes and neutron stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-594870