On the gravitational energy of the Hawking wormhole

Abstract

The surface energy for a conformally flat spacetime which represents the Hawking wormhole in spherical (static) Rindler coordinates is computed using the Hawking - Hunter formalism for non asymptotically - flat spacetimes. The physical gravitational Hamiltonian is proportional to the Rindler acceleration g of the hyperbolic observer and is finite on the event horizon ksi = b (b-the Planck length, ksi - the Minkowski interval). The corresponding temperature of the system of particles associated to the massless scalar field Psi, coupled conformally to Einstein's equations, is given by the Davies - Unruh temperature up to a constant factor of order unity.

9 pages, chapter 4 removed, to appear in Int. Jour. Mod. Phys. A

References in corpus (2)

• Some Heuristic Semiclassical Derivations of the Planck Length, the Hawking Effect and the Unruh Effect
• On boundary terms and conformal transformations in curved space-times

Cited by in corpus (5)

• Diamonds's Temperature: Unruh effect for bounded trajectories and thermal time hypothesis
• Is the Rindler horizon energy nonvanishing ?
• A brief remark on Unruh effect and causality
• Comments on "Thermodynamics and/of horizons : A comparison of Schwarzschild, Rindler and de Sitter spacetimes" (ArXiv : gr-qc/0202078), by T.Padmanabhan
• On the Hawking wormhole horizon entropy