Hawking Radiation from Plane Symmetric Black Hole Covariant Anomaly

AbstractA novel 4D Einstein–Gauss–Bonnet gravity was recently formulated by Glavan and Lin [Phys. Rev. Lett. 124, 081301 (2020)]. Although this theory may run into trouble at the level of action or equations of motion, the spherically symmetric black hole solution, which can be successfully reproduced in those consistent theories of 4D EGB gravity, is still meaningful and worthy of study. In this paper, we investigate Hawking radiation in the spacetime containing such a de Sitter black hole. Both the greybody factor and the power spectra of the Hawking radiation of the massless scalar are studied numerically for the full range of various parameters, including the GB coupling constant $$\alpha $$ α , the cosmological constant $$\Lambda $$ Λ and the coupling constant related to the scalar filed $$\xi $$ ξ . In particular, we find a negative $$\alpha $$ α leads to a larger greybody factor than that of a $$\alpha \ge 0$$ α ≥ 0 . While, for the power spectra of the Hawking radiation the situation is quite the opposite. The reason is that the temperature of the black hole would be very high when $$\alpha <0$$ α < 0 . Actually, we observe that the temperature would be arbitrarily high when $$\alpha $$ α approaches to the lower bound.

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HAWKING RADIATION OF DIRAC PARTICLES FROM A GENERAL DYNAMICAL SPHERICALLY SYMMETRICAL BLACK HOLE USING A NEW TORTOISE COORDINATE TRANSFORMATION

International Journal of Modern Physics D ◽

10.1142/s0218271814500308 ◽

2014 ◽

Vol 23 (04) ◽

pp. 1450030 ◽

Cited By ~ 1

Author(s):

JUN LIANG ◽

FANG-HUI ZHANG ◽

WEI ZHANG ◽

JING ZHANG

Keyword(s):

Black Hole ◽

Event Horizon ◽

Hawking Radiation ◽

Dirac Particles ◽

Tortoise Coordinate ◽

Temperature Parameter ◽

Undetermined Function ◽

Symmetric Black Hole ◽

Standard Wave ◽

New Tortoise Coordinate Transformation

By utilizing the improved Damour–Ruffini method with a new tortoise transformation, we study the Hawking radiation of Dirac particles from a general dynamical spherically symmetric black hole. In the improved Damour–Ruffini method, the position of the event horizon of the black hole is an undetermined function, and the temperature parameter κ is an undetermined constant. By requiring the Dirac equation to be the standard wave equation near the event horizon of the black hole, κ can be determined automatically. Therefore, the Hawking temperature can be obtained. The result is consistent with that of the Hawking radiation of scalar particles.

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The Spectroscopy of a Plane Symmetric Black Hole

International Journal of Theoretical Physics ◽

10.1007/s10773-013-1541-3 ◽

2013 ◽

Vol 52 (8) ◽

pp. 2560-2563

Author(s):

Deyou Chen ◽

Qiuping Zheng ◽

Jieyun Li ◽

Jie Zhang

Keyword(s):

Black Hole ◽

Plane Symmetric ◽

Symmetric Black Hole

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Quantum Tunnelling for Hawking Radiation from Both Static and Dynamic Black Holes

Advances in High Energy Physics ◽

10.1155/2014/168487 ◽

2014 ◽

Vol 2014 ◽

pp. 1-9 ◽

Cited By ~ 4

Author(s):

Subenoy Chakraborty ◽

Subhajit Saha

Keyword(s):

Black Hole ◽

Hawking Radiation ◽

Semiclassical Approximation ◽

Black Hole Entropy ◽

Jacobi Method ◽

Quantum Corrections ◽

Quantum Tunnelling ◽

Static Black Hole ◽

Symmetric Black Hole ◽

Correction Terms

The paper deals with Hawking radiation from both a general static black hole and a nonstatic spherically symmetric black hole. In case of static black hole, tunnelling of nonzero mass particles is considered and due to complicated calculations, quantum corrections are calculated only up to the first order. The results are compared with those for massless particles near the horizon. On the other hand, for dynamical black hole, quantum corrections are incorporated using the Hamilton-Jacobi method beyond semiclassical approximation. It is found that different order correction terms satisfy identical differential equation and are solved by a typical technique. Finally, using the law of black hole mechanics, a general modified form of the black hole entropy is obtained considering modified Hawking temperature.

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