Abstract

In the background of a gravitational collapse, we compute the transition amplitudes for the creation of particles for distant observers due to higher-derivative interactions in addition to Hawking radiation. The amplitudes grow exponentially with time and become of order 1 when the collapsing matter is about a Planck length outside the horizon. As a result, the effective theory breaks down at the scrambling time, invalidating its prediction of Hawking radiation. Planckian physics comes into play to decide the fate of black-hole evaporation.

Highlights

  • Planckian physics comes into play to decide the fate of black-hole evaporation

  • We consider outgoing particles with energies ∼ O(1/a) because states including them must exist in order for the effective theory to predict Hawking radiation. (Here, a ≡ 2GN M is the Schwarzschild radius, where GN is the Newton constant and M is the black hole mass.)

  • Because of this uncertainty principle, momentum conservation for freely falling observers hardly restricts the creation of outgoing particles for distant observers

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Summary

Review of scalar field in Schwarzschild background

We consider the gravitational collapse of a null thin shell at v = vs, so the metric (2.1) holds only for v ≥ vs. In the near-horizon region where 0 < r − a a, the Schwarzschild metric is approximately ds2 −dU dV + r2dΩ2,. We have used the same symbols (U, V ) for these coordinates because they can be identified with the Kruskal coordinates (2.4) and (2.5) across the collapsing shell in the near-horizon region. The creation-annihilation operators (a†Ω, aΩ) are defined with respect to the Kruskal coordinate U , and (b†ω, bω) those defined with respect to fiducial observers (or distant observers). They are related to each other via the Bogoliubov transformation bω =. Hawking radiation can be described in terms of 0|b†(ω0,u0)b(ω0,u0)|0 for a given wave packet, which is proportional to the Planck distribution [10]

Trans-Planckian problem
Energy conservation and uncertainty relation
Particle creation by higher-derivative interactions
Infalling particle radiation
Conclusion and discussion
Full Text
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