The thermodynamic theory of black holes

Details The thermodynamic theory of black holes The thermodynamic theory of black holes

Apr 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977rspsa.353..499d&link_type=abstract

Royal Society (London), Proceedings, Series A, vol. 353, no. 1675, Apr. 21, 1977, p. 499-521.

Astronomy and Astrophysics

Astrophysics

113

Astrophysics, Black Holes (Astronomy), Thermodynamic Properties, Energy Transfer, Entropy, Gravitational Collapse, Phase Transformations, Singularity (Mathematics), Specific Heat, Thermodynamic Equilibrium

Scientific paper

The thermodynamic theory underlying black-hole processes is developed in detail and applied to model systems. It is found that Kerr-Newman black holes undergo a phase transition at an angular-momentum mass ratio of 0.68M or an electric charge (Q) of 0.86M, where the heat capacity has an infinite discontinuity. Above the transition values the specific heat is positive, permitting isothermal equilibrium with a surrounding heat bath. Simple processes and stability criteria for various black hole situations are investigated. The limits for entropically favored black-hole formation are found. The Nernst conditions for the third law of thermodynamics are not satisfied fully for black holes. There is no obvious thermodynamic reason why a black hole may not be cooled down below absolute zero and converted into a naked singularity. Quantum energy-momentum tensor calculations for uncharged black holes are extended to the Reissner-Nordstrom case and found to be fully consistent with the thermodynamic picture for the case where electric charge is less than mass.

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