Trajectories of material particles in Kerr–Newman–de Sitter space–time

1989 ◽  
Vol 67 (5) ◽  
pp. 501-504
Author(s):  
K. D. Krori ◽  
Ranjana Choudhury ◽  
J. C. Sarmah
Keyword(s):  
Black Hole ◽  
Equatorial Plane ◽  
De Sitter Space ◽  
Space Time ◽  
De Sitter ◽  
Newman Black Hole

In this paper we show that in the Kerr–Newman–de Sitter space–time material particles may move in stable orbits in the equatorial plane (θ = π/2) of the Kerr–Newman black hole.

scholarly journals Hawking Non-thermal and Purely Thermal Radiations of Rotating Black Hole in Anti-de Sitter Space Time by Hamilton-Jacobi Method

2018 ◽  
Vol 37 ◽  
pp. 99-109
Author(s):  
M Ilias Hossain
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Emission Spectrum ◽  
Hawking Radiation ◽  
De Sitter Space ◽  
Space Time ◽  
Jacobi Method ◽  
De Sitter ◽  
Tunneling Method ◽  
Thermal Radiations

We have explored Hawking non-thermal and purely thermal radiations of Kerr-anti-de Sitter (KAdS) black hole using massive particles tunneling method by taking into account the space time background as dynamical, energy and angular momentum as conserved incorporating the selfgravitation effect of the emitted particles. The results we have obtained for KAdS black hole have shown that the tunneling rates are related to the change of Bekenstein-Hawking entropy and the derived emission spectrum deviates from the pure thermal spectrum and also the obtaining results for KAdS black hole are accordant with Parikh and Wilczek’s opinion and gives a correction to the Hawking radiation of KAdS black hole.GANIT J. Bangladesh Math. Soc.Vol. 37 (2017) 99-109

QUASINORMAL FREQUENCIES OF THE RARITA–SCHWINGER FIELD IN REISSNER–NORDSTRÖM-ANTI-DE SITTER SPACE–TIME

2006 ◽  
Vol 15 (06) ◽  
pp. 905-915 ◽  
Author(s):  
YUN ZHANG ◽  
JILIANG JING
Keyword(s):  
Black Hole ◽  
Quasinormal Modes ◽  
De Sitter Space ◽  
Space Time ◽  
Linear Functions ◽  
De Sitter ◽  
The Real ◽  
Large Black Hole ◽  
Angular Quantum Number ◽  
High Overtone

We investigate the quasinormal modes (QNMs) of Rarita–Schwinger field perturbations of a Reissner–Nordström black hole in an asymptotically anti-de Sitter space–time. We find that both the real and imaginary parts of the fundamental quasinormal frequencies of the large black hole are the linear functions of the Hawking temperature. The slope of the lines increases as the charge increases, but the imaginary parts decrease as the charge increases. We show that the quasinormal frequencies become evenly spaced for high overtone number n and the spacings are related to the charge and mass of the black hole. We also find that the real parts of the QNMs increase and the imaginary parts decrease as the angular quantum number increases.

Tunneling Radiation of a Torus-Like Black Hole in Anti-de Sitter Space-Time

2006 ◽  
Vol 45 (12) ◽  
pp. 2428-2436
Author(s):  
Hui-Ling Li ◽  
De-Jiang Qi ◽  
Qing-Quan Jiang ◽  
Shu-Zheng Yang
Keyword(s):  
Black Hole ◽  
De Sitter Space ◽  
Space Time ◽  
De Sitter ◽  
Tunneling Radiation

scholarly journals Black hole emission of vector particles in (1+1) dimensions

2014 ◽  
Vol 29 (22) ◽  
pp. 1450118 ◽  
Author(s):  
S. I. Kruglov
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Event Horizon ◽  
Quantum Tunneling ◽  
De Sitter Space ◽  
Space Time ◽  
De Sitter ◽  
Proca Equation ◽  
Scalar Particles ◽  
Vector Particles

We investigate the radiation of spin-1 particles by black holes in (1+1) dimensions within the Proca equation. The process is considered as quantum tunneling of bosons through an event horizon. It is shown that the emission temperature for the Schwarzschild background geometry is the same as the Hawking temperature corresponding to scalar particles emission. We also obtain the radiation temperatures for the de Sitter, Rindler and Schwarzschild–de Sitter space–times. In a particular case when two horizons in Schwarzschild–de Sitter space–time coincides, the Nariai temperature is recovered. The thermodynamical entropy of a black hole is calculated for Schwarzschild–de Sitter space–time having two horizons.

Fermion tunneling effect in Vaidya-de Sitter space

2010 ◽  
Vol 88 (4) ◽  
pp. 277-282 ◽  
Author(s):  
De-Jiang Qi ◽  
Wei-Min Wang ◽  
Shuang-Mei Li
Keyword(s):  
Black Hole ◽  
Energy Conservation ◽  
De Sitter Space ◽  
Space Time ◽  
Tunneling Probability ◽  
The Self ◽  
Tunneling Effect ◽  
De Sitter ◽  
Tunneling Method ◽  
Background Space

In this paper, by considering energy conservation and the self-gravitation reaction in the dynamical background space-time, we attempt to extend Kerner and Mann's work to the Vaidya–de Sitter black hole by the fermion-tunneling method. The result we derive shows that the tunneling probability of the Vaidya–de Sitter black hole is related not only to the change in the Bekenstein–Hawking entropy but also to the integral of the changing horizon, which are different from the stationary cases.

scholarly journals SEMICLASSICAL (QUANTUM FIELD THEORY) AND QUANTUM (STRING) DE SITTER REGIMES: NEW RESULTS

2007 ◽  
Vol 16 (06) ◽  
pp. 1053-1074 ◽  
Author(s):  
A. BOUCHAREB ◽  
M. RAMÓN MEDRANO ◽  
N. G. SÁNCHEZ
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Emission Cross Section ◽  
Hubble Constant ◽  
Flat Space ◽  
De Sitter Space ◽  
Space Time ◽  
De Sitter ◽  
Entropy Formula ◽  
New Phase

We compute the quantum string entropy S s (m, H) from the microscopic string density of states ρ s (m, H) of mass m in de Sitter space–time. We find for high m (high Hm → c/α') a new phase transition at the critical string temperature T s = (1/2πk B )L cl c2/α', higher than the flat space (Hagedorn) temperature t s (L cl = c/H, the Hubble constant H acts at the transition, producing a smaller string constant α' and thus, a higher tension). T s is the precise quantum dual of the semiclassical (QFT Hawking–Gibbons) de Sitter temperature T sem = ħ c/(2πk B L cl ). By precisely identifying the semiclassical and quantum (string) de Sitter regimes, we find a new formula for the full de Sitter entropy S sem (H), as a function of the usual Bekenstein–Hawking entropy [Formula: see text]. For L cl ≫ ℓ Planck , i.e. for low [Formula: see text] is the leading term, but for high H near c/ℓ Planck , a new phase transition operates and the whole entropy S sem (H) is drastically different from the Bekenstein–Hawking entropy [Formula: see text]. We compute the string quantum emission cross-section σ string by a black hole in de Sitter (or asymptotically de Sitter) space–time (bhdS). For T sem bhdS ℓ T s (early evaporation stage), it shows the QFT Hawking emission with temperature T sem bhdS (semiclassical regime). For T sem bhdS → T s , σ string exhibits a phase transition into a string de Sitter state of size [Formula: see text], [Formula: see text], and string de Sitter temperature T s . Instead of featuring a single pole singularity in the temperature (Carlitz transition), it features a square root branch point (de Vega–Sanchez transition). New bounds on the black hole radius r g emerge in the bhdS string regime: it can become r g = L s /2, or it can reach a more quantum value, r g = 0.365 ℓ s .

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