Abstract
We calculate the emission of gravitational waves, gravitons, photons and neutrinos from a perturbed Schwarzschild blackhole (BH). The perturbation can be due to either classical or quantum sources and therefore the injected energy can be either positive or negative. The emission can be classical in nature, as in the case of gravitational waves, or of quantum nature, for gravitons and the additional fields. We first set up the theoretical framework for calculating the emission by treating the case of a minimally coupled scalar field and then present the results for the other fields. We perform the calculations in the horizon-locking gauge in which the BH horizon is deformed, following similar calculations of tidal deformations of BH horizons. The classical emission can be interpreted as due to a partial exposure of a nonempty BH interior, while the quantum emission can be interpreted as an increased Hawking radiation flux due to the partial exposure of the BH interior. The degree of exposure of the BH interior is proportional to the magnitude of the injected null energy.
Highlights
Black holes (BHs) are well understood in the framework of general relativity (GR) where their semiclassical properties in the exterior region have been successfully described using the formalism of quantum fields in curved spacetime
Unlike the gravitational perturbations in classical GR, where radiation can only be emitted from a Schwarzschild BH in the form of gravitational waves, in the quantum case, due to coupling of the background metric to the various matter fields and their nonzero vacuum expectation value (VEV) of the stress energy momentum (SEM) tensor, gravitational perturbations produce additional particle species
We begin with the results that describe the classical gravitational wave emission from a perturbed Schwarzschild BH
Summary
Black holes (BHs) are well understood in the framework of general relativity (GR) where their semiclassical properties in the exterior region have been successfully described using the formalism of quantum fields in curved spacetime. Their quantum nature (in particular, quantum effects in the vicinity of the horizon) has not yet been fully understood and is inconsistent with the classical GR description. Unlike the gravitational perturbations in classical GR, where radiation can only be emitted from a Schwarzschild BH in the form of gravitational waves, in the quantum case, due to coupling of the background metric to the various matter fields and their nonzero VEV of the SEM tensor, gravitational perturbations produce additional particle species. For completeness, we explain in detail the relationship between our discussion of tidal deformations and the existing discussions in the literature
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