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The flaw in the firewall argument

By USA) OH 43210 Columbus The Ohio State University Samir D.(Department of Physics Mathur and USA) OH 43210 Columbus The Ohio State University David(Department of Physics Turton


A lot of confusion surrounds the issue of black hole complementarity, because the question has been considered without discussing the mechanism which guarantees unitarity. Considering such a mechanism leads to the following: (1) The Hawking quanta with energy E of order the black hole temperature T carry information, and so only appropriate processes involving <math altimg="si1.gif" xmlns=""><mi>E</mi><mo>≫</mo><mi>T</mi></math> quanta can have any possible complementary description with an information-free horizon; (2) The stretched horizon describes all possible black hole states with a given mass M , and it must expand out to a distance <math altimg="si2.gif" xmlns=""><msub><mrow><mi>s</mi></mrow><mrow><mtext><ce:italic>bubble</ce:italic></mtext></mrow></msub></math> before it can accept additional infalling bits; (3) The Hawking radiation has a specific low temperature T , and infalling quanta interact significantly with it only within a distance <math altimg="si3.gif" xmlns=""><msub><mrow><mi>s</mi></mrow><mrow><mi>α</mi></mrow></msub></math> of the horizon. One finds <math altimg="si4.gif" xmlns=""><msub><mrow><mi>s</mi></mrow><mrow><mi>α</mi></mrow></msub><mo>≪</mo><msub><mrow><mi>s</mi></mrow><mrow><mtext><ce:italic>bubble</ce:italic></mtext></mrow></msub></math> for <math altimg="si1.gif" xmlns=""><mi>E</mi><mo>≫</mo><mi>T</mi></math> , and this removes the argument against complementarity recently made by Almheiri et al. In particular, the condition <math altimg="si1.gif" xmlns=""><mi>E</mi><mo>≫</mo><mi>T</mi></math> leads to the notion of ‘fuzzball complementarity’, where the modes around the horizon are indeed correctly entangled in the complementary picture to give the vacuum

Year: 2014
DOI identifier: 10.1016/j.nuclphysb.2014.05.012
OAI identifier:

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