scholarly journals REGULAR AND BLACK HOLE SOLUTIONS TO HIGHER ORDER CURVATURE EINSTEIN–YANG–MILLS–GRASSMANNIAN SYSTEMS IN FIVE DIMENSIONS

2004 ◽  
Vol 19 (29) ◽  
pp. 5085-5096 ◽  
Author(s):  
YVES BRIHAYE ◽  
EUGEN RADU ◽  
D. H. TCHRAKIAN
Keyword(s):  
Black Hole ◽  
Critical Behavior ◽  
Sigma Model ◽  
Flat Space ◽  
Space Time ◽  
Matter Field ◽  
Spherically Symmetric ◽  
Five Dimensions ◽  
Yang Mills ◽  
Scalar Matter

Solutions to EYM systems in five space–time dimensions possessing no gravity decoupling limits, feature a peculiar critical behavior which is absent in their six-, seven- and eight-dimensional counterparts which do possess flat space limits. This critical behavior in five dimensions persists even when a scalar matter field is added, rendering the model nontrivial in the gravity decoupling limit. To this end, both regular and black hole spherically symmetric solutions to the higher curvature EYM–Grassmannian sigma model in d=5 space–time dimensions are constructed. A study of the solutions to the Grassmannian model in flat space is also carried out.

scholarly journals PROBING FOAMY SPACE–TIME WITH VARIATIONAL METHODS

1999 ◽  
Vol 14 (18) ◽  
pp. 2905-2920 ◽  
Author(s):  
REMO GARATTINI
Keyword(s):  
Black Hole ◽  
Variational Methods ◽  
Momentum Space ◽  
Flat Space ◽  
Casimir Energy ◽  
Space Time ◽  
Pair Creation ◽  
Variational Procedure ◽  
Loop Correction ◽  
Quasilocal Energy

A one-loop correction of the quasilocal energy in the Schwarzschild background, with flat space as a reference metric, is performed by means of a variational procedure in the Hamiltonian framework. We examine the graviton sector in momentum space, in the lowest possible state. An application to the black hole pair creation via the Casimir energy is presented. Implications on the foamlike scenario are discussed.

Super-Penrose process

2020 ◽  
Vol 35 (02n03) ◽  
pp. 2040058
Author(s):  
O. B. Zaslavskii
Keyword(s):  
Black Hole ◽  
Flat Space ◽  
Space Time ◽  
Centre Of Mass ◽  
Rotating Black Hole ◽  
Mass Frame ◽  
Penrose Process ◽  
Energy Formula ◽  
Full Classification

If two particles collide near a rotating black hole, their energy in the centre of mass frame can become unbounded under certain conditions. In doing so, the Killing energy [Formula: see text] of debris at infinity is, in general, remain restricted. If [Formula: see text] is also unbounded, this is called the super-Penrose process. We elucidate when such a process is possible and give full classification of corresponding relativistic objects for rotating space-times. We also discuss the case of a pure electric super-Penrose process that is valid even in the flat space-time. The key role in consideration is played by the Wald inequalities.

scholarly journals The Thermodynamic Relationship between the RN-AdS Black Holes and the RN Black Hole in Canonical Ensemble

2017 ◽  
Vol 2017 ◽  
pp. 1-7 ◽  
Author(s):  
Yu-Bo Ma ◽  
Li-Chun Zhang ◽  
Jian Liu ◽  
Ren Zhao ◽  
Shuo Cao
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Flat Space ◽  
Space Time ◽  
Asymptotically Flat ◽  
Time Space ◽  
Ads Black Holes ◽  
Different Types ◽  
Thermodynamic Relationship ◽  
The Relationship

In this paper, by analyzing the thermodynamic properties of charged AdS black hole and asymptotically flat space-time charged black hole in the vicinity of the critical point, we establish the correspondence between the thermodynamic parameters of asymptotically flat space-time and nonasymptotically flat space-time, based on the equality of black hole horizon area in the two different types of space-time. The relationship between the cavity radius (which is introduced in the study of asymptotically flat space-time charged black holes) and the cosmological constant (which is introduced in the study of nonasymptotically flat space-time) is determined. The establishment of the correspondence between the thermodynamics parameters in two different types of space-time is beneficial to the mutual promotion of different time-space black hole research, which is helpful to understand the thermodynamics and quantum properties of black hole in space-time.

scholarly journals EXTRA DIMENSIONS AND POSSIBLE SPACE-TIME SIGNATURE CHANGES

1995 ◽  
Vol 04 (04) ◽  
pp. 491-516 ◽  
Author(s):  
K.A. BRONNIKOV
Keyword(s):  
Black Hole ◽  
Extra Dimensions ◽  
Field Potential ◽  
Space Time ◽  
Spherically Symmetric ◽  
Vector Coupling ◽  
Special Cases ◽  
Dimensional Gravity ◽  
Time Changes ◽  
A Chain

Exact static, spherically symmetric solutions to the Einstein-Maxwell-scalar equations, with a dilatonic-type scalar-vector coupling, in D-dimensional gravity with a chain of n Ricci-flat internal spaces are considered, with the Maxwell field potential having two nonzero components: the temporal, Coulomb-like one and the one pointing to one of the extra dimensions. The properties and special cases of the solutions are discussed, in particular, those when there are horizons in the space-time. Two types of horizons are distinguished: the conventional black-hole (BH) ones and those at which the physical section of the space-time changes its signature (the latter are called T-horizons). Two theorems are proved, one fixing the BH- and T-horizon existence conditions, the other claiming that the system under study cannot have a regular center. The stability of a selected family of solutions under spherically symmetric perturbations is studied. It is shown that only black-hole solutions are stable, while all others, in particular, those with T-horizons are unstable.

scholarly journals Discussion of a Possible Corrected Black Hole Entropy

2018 ◽  
Vol 2018 ◽  
pp. 1-7 ◽  
Author(s):  
Miao He ◽  
Ziliang Wang ◽  
Chao Fang ◽  
Daoquan Sun ◽  
Jianbo Deng
Keyword(s):  
Black Hole ◽  
Electromagnetic Field ◽  
Black Hole Entropy ◽  
Einstein Gravity ◽  
Matter Field ◽  
Spherically Symmetric ◽  
Field Equations ◽  
Corrected Entropy ◽  
Entropy Of Black Hole ◽  
Spherically Symmetric Solution

Einstein’s equation could be interpreted as the first law of thermodynamics near the spherically symmetric horizon. Through recalling the Einstein gravity with a more general static spherical symmetric metric, we find that the entropy would have a correction in Einstein gravity. By using this method, we investigate the Eddington-inspired Born-Infeld (EiBI) gravity. Without matter field, we can also derive the first law in EiBI gravity. With an electromagnetic field, as the field equations have a more general spherically symmetric solution in EiBI gravity, we find that correction of the entropy could be generalized to EiBI gravity. Furthermore, we point out that the Einstein gravity and EiBI gravity might be equivalent on the event horizon. At last, under EiBI gravity with the electromagnetic field, a specific corrected entropy of black hole is given.

scholarly journals Asymptotically Lifshitz black hole solutions in F(R) gravity

2014 ◽  
Vol 92 (1) ◽  
pp. 76-81 ◽  
Author(s):  
S.H. Hendi ◽  
B. Eslam Panah ◽  
C. Corda
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Symmetric Space ◽  
Invariant Theory ◽  
Matter Field ◽  
Spherically Symmetric ◽  
Pure Gravity ◽  
Lifshitz Black Holes ◽  
Lifshitz Black Hole ◽  
Black Hole Solutions

We consider a class of spherically symmetric space–time to obtain some interesting solutions in F(R) gravity without matter field (pure gravity). We investigate the geometry of the solutions and find that there is an essential singularity at the origin. In addition, we show that there is an analogy between obtained solutions with the black holes of Einstein-Λ-power Maxwell invariant theory. Furthermore, we find that these solutions are equivalent to the asymptotically Lifshitz black holes. Also, we calculate d2F/dR2 to examine the Dolgov–Kawasaki stability criterion.

Sign in / Sign up

Export Citation Format

Share Document