Abstract
We address a long-standing problem of describing the thermodynamics of an accelerating black hole. We derive a standard first law of black hole thermodynamics, with the usual identification of entropy proportional to the area of the event horizon-even though the event horizon contains a conical singularity. This result not only extends the applicability of black hole thermodynamics to realms previously not anticipated, it also opens a possibility for studying novel properties of an important class of exact radiative solutions of Einstein equations describing accelerated objects. We discuss the thermodynamic volume, stability, and phase structure of these black holes.
Highlights
Black holes are possibly the most fascinating objects in our Universe
We derive a standard first law of black hole thermodynamics, with the usual identification of entropy proportional to the area of the event horizon—even though the event horizon contains a conical singularity. This result extends the applicability of black hole thermodynamics to realms previously not anticipated, it opens a possibility for studying novel properties of an important class of exact radiative solutions of Einstein equations describing accelerated objects
They provide a practical environment for testing strong gravity and are incredibly important theoretical tools for exploring Einstein’s general relativity (GR) and beyond
Summary
We derive a standard first law of black hole thermodynamics, with the usual identification of entropy proportional to the area of the event horizon—even though the event horizon contains a conical singularity This result extends the applicability of black hole thermodynamics to realms previously not anticipated, it opens a possibility for studying novel properties of an important class of exact radiative solutions of Einstein equations describing accelerated objects. They provide a practical environment for testing strong gravity and are incredibly important theoretical tools for exploring Einstein’s general relativity (GR) and beyond In spite of their central importance, the number of exact solutions describing a black hole is incredibly small; the Kerr-Newman family give us our prototypical black hole in four dimensions, and these are parametrized by mass, charge, and angular momentum.
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