From a collapsing radiating star to an evaporating black hole: A smooth transition from classical to quantum entropy

Abstract

We present a robust mechanism where the geometrical free-gravitational entropy of an isolated astrophysical radiating star undergoing continual gravitational collapse, as measured by an external observer, makes a smooth transition to the Bekenstein-Hawking entropy at the onset of the horizon formation and in the late times of black hole evaporation. It is interesting to note that both in the classical regime and the semi classical evaporating black hole regime, the matter is radiated via the Vaidya exterior surrounding the radiating star, as well as the evaporating black hole. Our result, being independent of the interior matter dynamics of the collapsing star, clearly indicates that the Bekenstein-Hawking entropy and its non-extensive nature indeed originates from the Riemannian geometry, which dictates the free-gravity entropy in general relativity.

arXiv comment5 pages, 1 figure

References in corpus (16)

• Primordial Black Holes
• Hawking Radiation and Black Hole Thermodynamics
• Gravito-electromagnetism
• A Multi-Mass Velocity Dispersion Model of 47 Tucanae Indicates No Evidence for an Intermediate Mass Black Hole
• A covariant approach for perturbations of rotationally symmetric spacetimes
• Covariant Perturbations of Schwarzschild Black Holes
• A Gravitational Entropy Proposal
• Scalar field and electromagnetic perturbations on Locally Rotationally Symmetric spacetimes
• Vaidya Space-Time in Black-Hole Evaporation
• Almost Birkhoff Theorem in General Relativity
• Astrophysical Black Hole horizons in a cosmological context: Nature and possible consequences on Hawking Radiation
• Birkhoff Theorem and Matter
• On the proximity of black hole horizons: lessons from Vaidya
• Constructing black hole entropy from gravitational collapse
• Transferring Energy in General Relativity
• Accreting Black Holes radiate classical Vaidya radiation to pave way for Hawking radiation