The geometric phase of a two-level atom under the Hawking effect in a Kerr black hole

2020 ◽  
Vol 37 (8) ◽  
pp. 085001
Author(s):  
Jiliang Jing ◽  
Zhipeng Cao ◽  
Xiaobao Liu ◽  
Zehua Tian
Keyword(s):  
Black Hole ◽  
Geometric Phase ◽  
Kerr Black Hole ◽  
Hawking Effect ◽  
Level Atom

QUANTUM THERMAL EFFECT OF ARBITRARILY ACCELERATING KERR BLACK HOLE

2005 ◽  
Vol 20 (07) ◽  
pp. 1353-1365
Author(s):  
XUEJUN YANG ◽  
ZHAO ZHENG
Keyword(s):  
Thin Film ◽  
Black Hole ◽  
Thermal Effect ◽  
Local Equilibrium ◽  
Kerr Black Hole ◽  
Black Hole Entropy ◽  
Static Case ◽  
Hawking Effect ◽  
Thin Film Model ◽  
Nonstationary Black Hole

By introducing a new Tortiose coordinate and using the notion of local equilibrium, we have studied the Hawking effect and the entropy of an arbitrarily accelerating Kerr black hole, a nonstationary black hole. The Bekenstein–Hawking entropy has been obtained by taking the same geometric cutoff relationship in the thin film model as that in the static case. Consequently, the results in the new Tortiose coordinate reveal the following two facts. First, it is correct in the opinion that the black hole entropy is determined by the horizon of a black hole, whether it is stationary or nonstationary. Second, the entropy of the nonstationary black hole shows some common essential natures with that of a static one.

scholarly journals Tortoise coordinate and Hawking effect in a dynamical Kerr black hole

2010 ◽  
Vol 331 (2) ◽  
pp. 627-631 ◽  
Author(s):  
Jian Yang ◽  
Zheng Zhao ◽  
Wenbiao Liu
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Hawking Effect ◽  
Tortoise Coordinate

GEOMETRIC PHASE AND DISENTANGLEMENT OF A MOVING FOUR-LEVEL ATOM IN THE PRESENCE OF NONLINEAR MEDIUM

2012 ◽  
Vol 10 (01) ◽  
pp. 1250007 ◽  
Author(s):  
NOUR ZIDAN ◽  
S. ABDEL-KHALEK ◽  
M. ABDEL-ATY
Keyword(s):  
System Dynamics ◽  
Geometric Phase ◽  
Nonlinear Medium ◽  
Atomic Motion ◽  
Kerr Medium ◽  
Mode Structure ◽  
Field Mode ◽  
Level Atom

In this paper, we investigate the geometric phase of the field interacting with a moving four-level atom in the presence of Kerr medium. The results show that the atomic motion, the field-mode structure and Kerr medium play important roles in the evolution of the system dynamics. As illustration, we examine the behavior of the geometric phase and entanglement with experimentally accessible parameters. Some new aspects are observed and discussed.

scholarly journals Choked accretion onto a Kerr black hole

2021 ◽  
Vol 103 (2) ◽  
Author(s):  
Alejandro Aguayo-Ortiz ◽  
Olivier Sarbach ◽  
Emilio Tejeda
Keyword(s):  
Black Hole ◽  
Kerr Black Hole

scholarly journals Influence of the geometric configuration of accretion flow on the black hole spin dependence of relativistic acoustic geometry

2018 ◽  
Vol 27 (03) ◽  
pp. 1850023 ◽  
Author(s):  
Pratik Tarafdar ◽  
Tapas K. Das
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Geometric Configuration ◽  
Surface Gravity ◽  
Linear Perturbation ◽  
Flow Profile ◽  
White Hole ◽  
Accretion Flow ◽  
Black Hole Spin ◽  
General Relativistic

Linear perturbation of general relativistic accretion of low angular momentum hydrodynamic fluid onto a Kerr black hole leads to the formation of curved acoustic geometry embedded within the background flow. Characteristic features of such sonic geometry depend on the black hole spin. Such dependence can be probed by studying the correlation of the acoustic surface gravity [Formula: see text] with the Kerr parameter [Formula: see text]. The [Formula: see text]–[Formula: see text] relationship further gets influenced by the geometric configuration of the accretion flow structure. In this work, such influence has been studied for multitransonic shocked accretion where linear perturbation of general relativistic flow profile leads to the formation of two analogue black hole-type horizons formed at the sonic points and one analogue white hole-type horizon which is formed at the shock location producing divergent acoustic surface gravity. Dependence of the [Formula: see text]–[Formula: see text] relationship on the geometric configuration has also been studied for monotransonic accretion, over the entire span of the Kerr parameter including retrograde flow. For accreting astrophysical black holes, the present work thus investigates how the salient features of the embedded relativistic sonic geometry may be determined not only by the background spacetime, but also by the flow configuration of the embedding matter.

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