Quantum-gravity fluctuations and the black-hole temperature

The European Physical Journal C

Shahar Hod¹ 

[1] The Ruppin Academic Center, 40250, Emeq Hefer, Israel;The Hadassah Institute, 91010, Jerusalem, Israel;

关键词: Black Hole;    Area Spectrum;    Quantum Black Hole;    Quantum Entity;    Gravitational Resonance;   

DOI  :  10.1140/epjc/s10052-015-3465-y

来源: Springer

【 摘 要 】

Bekenstein has put forward the idea that, in a quantum theory of gravity, a black hole should have a discrete energy spectrum with concomitant discrete line emission. The quantized black-hole radiation spectrum is expected to be very different from Hawking’s semi-classical prediction of a thermal black-hole radiation spectrum. One naturally wonders: Is it possible to reconcile the discrete quantum spectrum suggested by Bekenstein with the continuous semi-classical spectrum suggested by Hawking? In order to address this fundamental question, in this essay we shall consider the zero-point quantum-gravity fluctuations of the black-hole spacetime. In a quantum theory of gravity, these spacetime fluctuations are closely related to the characteristic gravitational resonances of the corresponding black-hole spacetime. Assuming that the energy of the black-hole radiation stems from these zero-point quantum-gravity fluctuations of the black-hole spacetime, we derive the effective temperature of the quantized black-hole radiation spectrum. Remarkably, it is shown that this characteristic temperature of the discrete (quantized) black-hole radiation agrees with the well-known Hawking temperature of the continuous (semi-classical) black-hole spectrum.

【 授权许可】

CC BY