Some quantum gravity theories, like Loop Quantum Gravity, predict that quantum mechanical effects will avoid the formation of a singularity inside a black hole. From the general relativity point of view, this means that the metric will differ from the ones of Schwarzschild or Kerr at least inside the event horizon. If the metric is not that of Schwarzschild or Kerr, the potential of the Regge-Wheeler equation is modified, therefore it is possible to peek inside a black hole using the Quasi-Normal Modes to find out if there is indeed a singularity. We address this problem for a regular Schwartzchild black hole using an effective metric first introduced by Hayward.
Quasi-normal mode of a regular Schwarzschild black hole
Mattia Villani
2020
Abstract
Some quantum gravity theories, like Loop Quantum Gravity, predict that quantum mechanical effects will avoid the formation of a singularity inside a black hole. From the general relativity point of view, this means that the metric will differ from the ones of Schwarzschild or Kerr at least inside the event horizon. If the metric is not that of Schwarzschild or Kerr, the potential of the Regge-Wheeler equation is modified, therefore it is possible to peek inside a black hole using the Quasi-Normal Modes to find out if there is indeed a singularity. We address this problem for a regular Schwartzchild black hole using an effective metric first introduced by Hayward.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
