Hawking Radiation from the Horowitz--Strominger Black Hole

Chin. Phys. Lett.

2005, Vol. 22

Issue (7): 1611-1613 DOI:

Original Articles

Hawking Radiation from the Horowitz--Strominger Black Hole

FANG Heng-Zhong^1,2;HU Ya-Peng²;ZHAO Zheng²

¹Department of Physics, Chinese Ocean University, Qingdao 266071 ²Department of Physics, Beijing Normal University, Beijing 100875

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FANG Heng-Zhong, HU Ya-Peng, ZHAO Zheng 2005 Chin. Phys. Lett. 22 1611-1613

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Abstract When a black hole radiates particles, it losses energy and shrinks, the horizon contracts from its original radius to a new smaller radius. This leads to the separation between the initial and final radii, which sets the barrier for the particles to tunnel. We develop the work of Parikh [Phys. Rev. Lett. 85(2000)5042; Gen. Rel. Grav. 36,(2004)2419] to a Horowitz--Strominger black hole, i.e. applying the Wentzel--Kramers--Brillouin approximation and semi-classical method to calculate the rate of the Hawking radiation. The result agrees with Γ ～ e^-2ImI=e^ΔS_BH. It is also proven that the energy spectrum deviates from exact thermality.

Keywords: 04.70.Dy 04.70.Bw

Published: 01 July 2005

PACS:	04.70.Dy	(Quantum aspects of black holes, evaporation, thermodynamics)
	04.70.Bw	(Classical black holes)

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https://cpl.iphy.ac.cn/ OR https://cpl.iphy.ac.cn/Y2005/V22/I7/01611

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