2004/04/30 by Sean A. Hayward · 1 citation
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Classical mechanics #Conservation law #Cosmology and Gravitation Theories #Energy flux #Geometry #Gravitation #Gravitational energy #Gravitational wave #Hawking radiation #Negative energy #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Tensor (intrinsic definition) #gr-qc
paper · pdf · doi:10.1103/physrevlett.93.251101
published as Phys.Rev.Lett.93:251101,2004 · 4 revtex4 pages. Many (mostly presentational) changes; emphasizes the definition of gravitational radiation in the strong-field regime
arxiv created 2004/08/03 · openalex publication_date 2004/12/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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. This first law of black-hole dynamics describes how a black hole grows and is regular in the limit where it 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 of a stationary Killing vector. Identifying an energy flux, vanishing if and only if the horizon is null, allows a division into energy supply and work terms. The energy supply can be expressed in terms of area increase and a newly defined surface gravity, yielding a Gibbs-like equation.