Phenomenology of GUP stars
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Regular Article - Theoretical Physics
Phenomenology of GUP stars Luca Buoninfante1,a , Gaetano Lambiase2,3,b , Giuseppe Gaetano Luciano2,3,c , Luciano Petruzziello2,4,d 1
Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan INFN, Sezione di Napoli, Gruppo collegato di Salerno, Fisciano, SA 84084, Italy 3 Dipartimento di Fisica, Università di Salerno, Fisciano, SA 84084, Italy 4 Dipartimento di Ingegneria, Università di Salerno, Fisciano, SA 84084, Italy
2
Received: 20 February 2020 / Accepted: 4 September 2020 © The Author(s) 2020
Abstract We study quantum corrections at the horizon scale of a black hole induced by a Generalized Uncertainty Principle (GUP) with a quadratic term in the momentum. The interplay between quantum mechanics and gravity manifests itself into a non-zero uncertainty in the location of the black hole radius, which turns out to be larger than the usual Schwarzschild radius. We interpret such an effect as a correction which makes the horizon disappear, as it happens in other models of quantum black holes already considered in literature. We name this kind of horizonless compact objects GUP stars. We also investigate some phenomenological aspects in the astrophysical context of binary systems and gravitational wave emission by discussing Love numbers, quasi-normal modes and echoes, and studying their behavior as functions of the GUP deformation parameter. Finally, we preliminarily explore the possibility to constrain such a parameter with future astrophysical experiments.
1 Introduction Einstein’s general relativity (GR) turns out to be the best description of the gravitational interaction so far. Its predictions have been tested to very high precision at large distances and late times [1]; just to mention the most recent experimental confirmations, we can think of the detection of gravitational waves (GWs) from a binary black hole merger [2,3] and the capture of the first black hole image [4]. However, despite its great success, there are still conceptual problems which are plaguing the theory and no satisfactory solution has been found up today. Indeed, GR admits black hole solutions which suffer from curvature singularity and possess a a e-mail:
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horizon, and both these features cause troubles when shortdistances are considered [5] and/or quantization in curved spacetime is implemented [6–8]. To be more precise, we have not seen any black hole experimentally, but only dark objects which behave very similarly to them, thus allowing for the existence of many alternative descriptions still not excluded by observations. In order for a theory of gravity to be consistent, no singularity or paradox should arise. Recent investigations have shown that a resolution to the information loss paradox [7,8] can be found by assuming that the effective radius of the astrophysical object is larger than the corresponding horizon
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