Loop quantum Schwarzschild interior and black hole remnant

We present the state of the art regarding the relation between the physics of Quantum Black Holes and Noncommutative Geometry. We start with a review of models proposed in the literature for describing deformations of General Relativity in the presence of noncommutativity, seen as an effective theory of Quantum Gravity. We study the resulting metrics, proposed to replace or at least to improve the conventional black hole solutions of Einstein's equation. In particular, we analyze noncommutative-inspired solutions obtained in terms of quasiclassical noncommutative coordinates: indeed because of their surprising new features, these solutions enable us to circumvent long standing problems with Quantum Field Theory in Curved Space and to cure the singular behavior of gravity at the centers of black holes. As a consequence, for the first time, we get a complete description of what we may call the black hole SCRAM, the shut down of the emission of thermal radiation from the black hole: in place of the conventional scenario of runaway evaporation in the Planck phase, we find a zero temperature final state, a stable black hole remnant, whose size and mass are determined uniquely in terms of the noncommutative parameter θ. This result turns out to be of vital importance for the physics of the forthcoming experiments at the LHC, where mini black hole production is foreseen in extreme energy hadron collisions. Because of this, we devote the final part of this review to higher-dimensional solutions and their phenomenological implications for TeV Gravity.

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Black hole remnant and quantum tunnelling in three-dimensional Gödel spacetime

Astrophysics and Space Science ◽

10.1007/s10509-015-2316-5 ◽

2015 ◽

Vol 357 (1) ◽

Cited By ~ 7

Author(s):

Hui-Ling Li ◽

Xiao-Tao Zu

Keyword(s):

Black Hole ◽

Three Dimensional ◽

Quantum Tunnelling ◽

Black Hole Remnant

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GUP-corrected thermodynamics of accelerating and rotating black holes

International Journal of Modern Physics D ◽

10.1142/s0218271817410188 ◽

2017 ◽

Vol 26 (05) ◽

pp. 1741018 ◽

Cited By ~ 5

Author(s):

Muhammad Rizwan ◽

K. Saifullah

Keyword(s):

Black Holes ◽

Black Hole ◽

Quantum Gravity ◽

Black Hole Physics ◽

Generalized Uncertainty Principle ◽

Hawking Temperature ◽

Rotating Black Holes ◽

Gravity Effects ◽

Klein Gordon ◽

Black Hole Remnant

When quantum gravity effects, that are based on generalized uncertainty principle with a minimal measurable length, are incorporated into black hole physics the Klein–Gordon and Dirac equations get modified. Using these modified equations we investigate tunneling of scalar particles and fermions from event and acceleration horizons of accelerating and rotating black holes and obtain the modified Hawking temperature with quantum gravity effects. We see that Hawking temperature depends on black hole parameters as well as the quantum numbers of emitted fermions. The quantum corrections slow down black hole evaporation and leave a black hole remnant. This contradicts complete evaporation of a black hole which is presaged by the standard temperature formula for black holes. The modified Hawking temperatures presented here, in appropriate limits, are consistent with the previous results in the literature.

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Simulations of Recoiling Massive Black Holes

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310006393 ◽

2009 ◽

Vol 5 (S267) ◽

pp. 262-262

Author(s):

Javiera Guedes ◽

Piero Madau ◽

Lucio Mayer ◽

Michael Kuhlen ◽

Jürg Diemand ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Return Time ◽

Wave Radiation ◽

Host Galaxy ◽

Massive Black Holes ◽

Black Hole Binaries ◽

The Galaxy ◽

Central Regions ◽

Black Hole Remnant

AbstractThe coalescence of black hole binaries is a significant source of gravitational wave radiation. The typically asymmetric nature of this emission, which carries linear momentum, can result in the recoil of the black hole remnant with velocities in the range 100 < Vrecoil < 3750 km s−1. The detectability of recoiling massive black holes (MBH) as off-nuclear QSOs is tightly connected with the properties of the host galaxy, which determine the MBH's orbit and fuel reservoir. We present the results of N-body simulations of recoiling MBHs in high-resolution, non-axisymmetric potentials. We find that if the recoil velocities are high enough to reach regions of the galaxy dominated by the generally triaxial dark matter distribution, the return time is significantly extended when compared to a spherical distribution. We also perform simulations of recoiling MBHs traveling in gas merger remnants, where large amounts of gas have been funneled to the central regions, In this case, the MBHs remain within R<1 kpc from the center of the host even for high recoil velocities (Vrecoil = 1200 km s−1) due to the compactness of the remnant galaxy's nuclear disk. We discuss the implications of both scenarios for detectability.

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