Beyond the semi-classical description of black hole evaporation
| dc.creator | Parentani, Renaud | |
| dc.date | 2007-04-19 | |
| dc.date.accessioned | 2026-07-07T11:28:39Z | |
| dc.date.available | 2026-07-07T11:28:39Z | |
| dc.description | In the semi-classical treatment, i.e. in a classical black hole geometry, Hawking quanta emerge from trans-Planckian configurations because of scale invariance. There is indeed no scale to stop the blue-shifting effect encountered in the backward propagation towards the event horizon. On the contrary, when taking into account the gravitational interactions neglected in the semi-classical treatment, a UV scale stopping the blue-shift could be dynamically engendered. To show that this is the case, we use a non-perturbative treatment based on the large-N limit, where $N$ is the number of matter fields. In this limit, the semi-classical treatment is the leading contribution. Non-linear gravitational effects appear in the next orders and in the first of these, the effects are governed by the two-point correlation function of the energy-momentum tensor evaluated in the vacuum. Taking this correlator into account, backward propagated modes are dissipated at a distance from the horizon $\propto Gκ$ when measured in a freely falling frame. ($G$ is Newton's constant and $κ$ the surface gravity.) This result can be also obtained by considering light propagation in a stochastic ensemble of metrics whose fluctuations are determined by the above correlator. | |
| dc.description | 26 pages, 1 figure, revised and updated version | |
| dc.identifier | https://arxiv.org/abs/0704.2563 | |
| dc.identifier | http://arxiv.org/abs/0704.2563 | |
| dc.identifier | Int.J.Theor.Phys.41:2175-2200,2002 | |
| dc.identifier | doi:10.1023/A:1021133126804 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/196460 | |
| dc.subject | High Energy Physics - Theory | |
| dc.title | Beyond the semi-classical description of black hole evaporation | |
| dc.type | text |