scholarly journals Higher derivative corrections to BPS black hole attractors in 4d gauged supergravity

2016 ◽  
Vol 2016 (5) ◽  
Author(s):  
Kiril Hristov ◽  
Stefanos Katmadas ◽  
Ivano Lodato
Keyword(s):  
Black Hole ◽  
Higher Derivative ◽  
Black Hole Attractors

scholarly journals Black Hole Attractors in Extended Supergravity

2007 ◽  
Author(s):  
Sergio Ferrara ◽  
Alessio Marrani ◽  
Arttu Rajantie ◽  
Carlo Contaldi ◽  
Paul Dauncey ◽  
...  
Keyword(s):  
Black Hole ◽  
Black Hole Attractors

scholarly journals Black hole evaporation in Hořava–Lifshitz gravity

2020 ◽  
Vol 80 (7) ◽  
Author(s):  
Hao Xu ◽  
Yen Chin Ong
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Lorentz Invariance ◽  
Detailed Balance ◽  
Einstein Gravity ◽  
Zero Temperature ◽  
Black Hole Mass ◽  
Black Hole Evaporation ◽  
Higher Derivative ◽  
Temperature State

Abstract Hořava–Lifshitz (HL) gravity was formulated in hope of solving the non-renormalization problem in Einstein gravity and the ghost problem in higher derivative gravity theories by violating Lorentz invariance. In this work we consider the spherically symmetric neutral AdS black hole evaporation process in HL gravity in various spacetime dimensions d, and with detailed balance violation parameter $$0\leqslant \epsilon ^2\leqslant 1$$0⩽ϵ2⩽1. We find that the lifetime of the black holes under Hawking evaporation is dimensional dependent, with $$d=4,5$$d=4,5 behave differently from $$d\geqslant 6$$d⩾6. For the case of $$\epsilon =0$$ϵ=0, in $$d=4,5$$d=4,5, the black hole admits zero temperature state, and the lifetime of the black hole is always infinite. This phenomenon obeys the third law of black hole thermodynamics, and implies that the black holes become an effective remnant towards the end of the evaporation. As $$d\geqslant 6$$d⩾6, however, the lifetime of black hole does not diverge with any initial black hole mass, and it is bounded by a time of the order of $$\ell ^{d-1}$$ℓd-1, similar to the case of Schwarzschild-AdS in Einstein gravity (which corresponds to $$\epsilon ^2=1$$ϵ2=1), though for the latter this holds for all $$d\geqslant 4$$d⩾4. The case of $$0<\epsilon ^2<1$$0<ϵ2<1 is also qualitatively similar with $$\epsilon =0$$ϵ=0.

scholarly journals D0-branes in black hole attractors

2006 ◽  
Vol 2006 (03) ◽  
pp. 019-019 ◽  
Author(s):  
Davide Gaiotto ◽  
Aaron Simons ◽  
Andrew Strominger ◽  
Xi Yin
Keyword(s):  
Black Hole ◽  
Black Hole Attractors

scholarly journals Black Hole Entropy for Two Higher Derivative Theories of Gravity

Entropy ◽  
2010 ◽  
Vol 12 (10) ◽  
pp. 2186-2198 ◽  
Author(s):  
Emilio Bellini ◽  
Roberto Di Criscienzo ◽  
Lorenzo Sebastiani ◽  
Sergio Zerbini
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Higher Derivative ◽  
Theories Of Gravity

scholarly journals Black-hole attractors inN= 1 supergravity

2007 ◽  
Vol 2007 (07) ◽  
pp. 019-019 ◽  
Author(s):  
Laura Andrianopoli ◽  
Riccardo D'Auria ◽  
Sergio Ferrara ◽  
Mario Trigiante
Keyword(s):  
Black Hole ◽  
Black Hole Attractors

scholarly journals Black hole attractors and pure spinors

2006 ◽  
Vol 2006 (09) ◽  
pp. 048-048 ◽  
Author(s):  
Jonathan P Hsu ◽  
Alexander Maloney ◽  
Alessandro Tomasiello
Keyword(s):  
Black Hole ◽  
Black Hole Attractors

scholarly journals Planckian physics comes into play at Planckian distance from horizon

2022 ◽  
Vol 2022 (1) ◽  
Author(s):  
Pei-Ming Ho ◽  
Hikaru Kawai ◽  
Yuki Yokokura
Keyword(s):  
Black Hole ◽  
Gravitational Collapse ◽  
Hawking Radiation ◽  
Effective Theory ◽  
Planck Length ◽  
Black Hole Evaporation ◽  
Higher Derivative ◽  
The Creation ◽  
Transition Amplitudes

Abstract In the background of a gravitational collapse, we compute the transition amplitudes for the creation of particles for distant observers due to higher-derivative interactions in addition to Hawking radiation. The amplitudes grow exponentially with time and become of order 1 when the collapsing matter is about a Planck length outside the horizon. As a result, the effective theory breaks down at the scrambling time, invalidating its prediction of Hawking radiation. Planckian physics comes into play to decide the fate of black-hole evaporation.

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