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Relativity, Gravitation and CosmologyA Basic Introduction$
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Ta-Pei Cheng

Print publication date: 2009

Print ISBN-13: 9780199573639

Published to Oxford Scholarship Online: February 2010

DOI: 10.1093/acprof:oso/9780199573639.001.0001

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Black holes

Black holes

Chapter:
(p.141) 8 Black holes
Source:
Relativity, Gravitation and Cosmology
Author(s):

Ta-Pei Cheng

Publisher:
Oxford University Press
DOI:10.1093/acprof:oso/9780199573639.003.0008

Black hole is an object so compact that it is inside its event horizon: a one-way surface through which particle and light can only traverse inward, and an exterior observer cannot receive any signal sent from inside. The Schwarzschild geometry is viewed in the Eddington-Finkelstein coordinates as well as in the Kruskal coordinates. Besides a black hole, the GR field equation also allows the solution of a white hole and a wormhole. The gravitational energy released when a particle falls into a tightly bound orbit around a black hole can be enormous. The physical reality of, and observational evidence for, black holes are briefly discussed. Quantum fluctuation around the event horizon brings about the Hawking radiation. This and the Penrose process in a rotating (Kerr) black hole comes about because of the possibility of negative energy particles falling into a black hole.

Keywords:   black holes, white holes, wormholes, Eddington-Finkelstein, Kruskal coordinates, Kerr metric, gravitational binding energy, Hawking radiation, Penrose process, quantum fluctuation, negative energy, rotating black hole

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