scholarly journals Quantum gravity corrections to accretion onto a Schwarzschild black hole

2015 ◽  
Vol 92 (8) ◽  
Author(s):  
Rongjia Yang
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Schwarzschild Black Hole

Effect of post-Newtonian-like self-energy, quantum gravity and exchange correlations on Schwarzschild black hole: Application of uncertainty principle

2020 ◽  
Vol 35 (11) ◽  
pp. 2050081
Author(s):  
Baljeet Kaur Lotte ◽  
Subodha Mishra
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Correlation Energy ◽  
Particle System ◽  
Gravitational Interaction ◽  
Schwarzschild Black Hole ◽  
Loop Contribution ◽  
Exchange Correlation ◽  
Self Energy ◽  
Energy Quantum

The expressions for the corrected radius and the Hawking temperature of a Schwarzschild black hole are derived by calculating the total energy of a self-gravitating system of N fermions when the corrections to gravitational interaction due to post-Newtonian-like self-energy due to two graviton exchange- and one-loop contribution of quantum gravity effect are included. Since the particles are fermions, the exchange-correlation energy is also included consistently. It is found that though the three corrections are small, the correction due to the exchange-correlation is much more than the other two. The configuration of the many-particle system that we study is possible since it has no Buchdahl limit in the post-Newtonian approximation.

scholarly journals Accretion disk around a Schwarzschild black hole in asymptotic safety

2021 ◽  
Vol 81 (9) ◽  
Author(s):  
Fabián H. Zuluaga ◽  
Luis A. Sánchez
Keyword(s):  
Black Hole ◽  
Thermal Properties ◽  
Quantum Gravity ◽  
Schwarzschild Black Hole ◽  
Spacetime Geometry ◽  
Black Hole Candidate ◽  
Stable Circular Orbit ◽  
Gravity Effects ◽  
Relativistic Regime ◽  
Higher Derivatives

AbstractWe study quantum gravity effects on radiation properties of thin accretion disks around a renormalization group improved (RGI-) Schwarzschild black hole. In the infrared (IR) limit of the asymptotically safe theory with higher derivatives, the running Newton coupling G(r) depends on a free parameter which encodes the quantum effects on the spacetime geometry. By varying this parameter, modifications to thermal properties of the disk as the time averaged energy flux, the disk temperature, the differential luminosity, and the conversion efficiency of accreting mass into radiation, are obtained. In addition to a shifting of the radius of the innermost stable circular orbit (ISCO) toward small values, we find an increase of the maximum values of these thermal properties and a greater efficiency than in the classical relativistic regime. We discuss astrophysical applications of these results by using observational data of the stellar-mass black hole candidate LMC X-3. Our findings could, in principle, be used to identify quantum gravity effects through astrophysical observations.

scholarly journals Schwarzschild black hole states and entropies on a nice slice

2020 ◽  
Vol 80 (12) ◽  
Author(s):  
J. A. Rosabal
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Pure State ◽  
Entanglement Entropy ◽  
The State ◽  
Schwarzschild Black Hole ◽  
Complex Time ◽  
Strong Curvature

AbstractIn this work, we define a quantum gravity state on a nice slice. The nice slices provide a foliation of spacetime and avoid regions of strong curvature. We explore the topology and the geometry of the manifold obtained from a nice slice after evolving it in complex time. We compute its associated semiclassical thermodynamics entropy for a 4d Schwarzschild black hole. Despite the state one can define on a nice slice is not a global pure state, remarkably, we get a similar result to Hawking’s calculation. In the end, we discuss the entanglement entropy of two segments on a nice slice and comment on the relation of this work with the replica wormhole calculation.

scholarly journals A consistent model of non-singular Schwarzschild black hole in loop quantum gravity and its quasinormal modes

2020 ◽  
Vol 2020 (07) ◽  
pp. 066-066 ◽  
Author(s):  
Mariam Bouhmadi-López ◽  
Suddhasattwa Brahma ◽  
Che-Yu Chen ◽  
Pisin Chen ◽  
Dong-han Yeom
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Loop Quantum Gravity ◽  
Quasinormal Modes ◽  
Schwarzschild Black Hole ◽  
Consistent Model

Dirac quasi-normal frequencies in a noncommutative black hole space–time

2019 ◽  
Vol 97 (5) ◽  
pp. 562-565
Author(s):  
Cuibai Luo ◽  
Chen Wu
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Noncommutative Geometry ◽  
Imaginary Part ◽  
Normal Modes ◽  
Space Time ◽  
Numerical Results ◽  
Schwarzschild Black Hole ◽  
Oscillation Frequencies ◽  
Noncommutative Parameter

Noncommutative geometry may be an alternative way to quantum gravity. We study the influence of the space–time noncommutative parameter on the Dirac quasi-normal modes in the noncommutative Schwarzschild black hole space–times. In comparison to the commutative Schwarzschild black hole, the numerical results show that the oscillation frequencies and magnitude of the imaginary part of the Dirac quasi-normal modes will increase. However, it is found that the influence of the space–time noncommutative parameter on the Dirac quasi-normal modes is tiny and negligible.

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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