TY - JOUR

T1 - Hawking radiation of a quantum black hole in an inflationary universe

AU - Huang, Wung Hong

PY - 1992

Y1 - 1992

N2 - The quantum stress-energy tensor of a massless scalar field propagating in the two-dimensional Vaidya-de Sitter metric, which describes a classical model spacetime for a dynamical evaporating black hole in an inflationary universe, is analysed. The author presents a possible way to obtain the Hawking radiation terms for the model with arbitrary functions of mass. It is used to see how the expansion of universe will affect the dynamical process of black-hole evaporation. The results show that the cosmological inflation has an inclination to depress the black hole evaporation. However, if the cosmological constant is sufficiently large then the back-reaction effect has the inclination to increase the black-hole evaporation. He also presents a simple method to show that it will always produce a divergent flux of outgoing radiation along the Cauchy horizon where the curvature is a finite value. This means that the Hawking radiation will be very large in there and shall modify classical spacetime drastically. Therefore black hole evaporation cannot be discussed self-consistently on the classical Vaidya-type spacetime. The method can also be applied to analyse the quantum stress-energy tensor in the more general Vaidya-type spacetimes.

AB - The quantum stress-energy tensor of a massless scalar field propagating in the two-dimensional Vaidya-de Sitter metric, which describes a classical model spacetime for a dynamical evaporating black hole in an inflationary universe, is analysed. The author presents a possible way to obtain the Hawking radiation terms for the model with arbitrary functions of mass. It is used to see how the expansion of universe will affect the dynamical process of black-hole evaporation. The results show that the cosmological inflation has an inclination to depress the black hole evaporation. However, if the cosmological constant is sufficiently large then the back-reaction effect has the inclination to increase the black-hole evaporation. He also presents a simple method to show that it will always produce a divergent flux of outgoing radiation along the Cauchy horizon where the curvature is a finite value. This means that the Hawking radiation will be very large in there and shall modify classical spacetime drastically. Therefore black hole evaporation cannot be discussed self-consistently on the classical Vaidya-type spacetime. The method can also be applied to analyse the quantum stress-energy tensor in the more general Vaidya-type spacetimes.

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U2 - 10.1088/0264-9381/9/5/004

DO - 10.1088/0264-9381/9/5/004

M3 - Article

AN - SCOPUS:33750430301

SN - 0264-9381

VL - 9

SP - 1199

EP - 1209

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

IS - 5

M1 - 004

ER -