Quasi-homogeneous black hole thermodynamics

Black Hole thermodynamics without a black hole?

In the present paper we consider, using our earlier results, the process of quantum gravitational collapse and argue that there exists the final quantum state when the collapse stops. This state, which can be called the “no-memory state”, reminds the final “no-hair state” of the classical gravitational collapse. Translating the “no-memory state” into classical language we construct the classica...

Quasi-classical Hawking Temperatures and Black Hole Thermodynamics

The semi-classical derivation of Hawking radiation for axially symmetric, stationary spacetimes with a Killing horizon is examined following the recent quasi-classical tunneling analysis [1] and a simple formula is found for the inverse Hawking temperature β = 1/TH . The formula is invariant under canonical transformations and is shown to be equivalent to the integral of a closed differential 1...

Noncommutative Black Hole Thermodynamics

We give a general (metric independent) derivation of the relation Th = K 2π connecting the black hole temperature (Th) with the surface gravity (K), following the tunneling interpretation of Hawking radiation. This derivation is valid even beyond the semi classical regime i. e. when quantum effects are not negligible. The formalism is then applied to a spherically symmetric, stationary noncommu...

Black hole thermodynamics

These notes introduce basic aspects of black hole thermodynamics. I review the classical laws of black hole mechanics, give a brief introduction to the essential concepts of quantum field theory in curved spacetime, and derive the Unruh and Hawking effects. I conclude with a discussion of entropy from the Euclidean path integral point of view and in the context of the AdS/CFT correspondence. Or...

Black Hole Thermodynamics ∗