Energy conservation for dynamical black holes

Details Energy conservation for dynamical black holes Energy conservation for dynamical black holes

2004-04-18

arxiv.org/abs/gr-qc/0404077v2

Phys.Rev.Lett.93:251101,2004

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

4 revtex4 pages. Many (mostly presentational) changes; emphasizes the definition of gravitational radiation in the strong-fiel

Scientific paper

10.1103/PhysRevLett.93.251101

An energy conservation law is described, expressing the increase in mass-energy of a general black hole in terms of the energy densities of the infalling matter and gravitational radiation. For a growing black hole, this first law of black-hole dynamics is equivalent to an equation of Ashtekar & Krishnan, but the new integral and differential forms are regular in the limit where the black hole ceases to grow. An effective gravitational-radiation energy tensor is obtained, providing measures of both ingoing and outgoing, transverse and longitudinal gravitational radiation on and near a black hole. Corresponding energy-tensor forms of the first law involve a preferred time vector which plays the role for dynamical black holes which the stationary Killing vector plays for stationary black holes. Identifying an energy flux, vanishing if and only if the horizon is null, allows a division into energy-supply and work terms, as in the first law of thermodynamics. The energy supply can be expressed in terms of area increase and a newly defined surface gravity, yielding a Gibbs-like equation, with a similar form to the so-called first law for stationary black holes.

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