scholarly journals Holographic Brownian Motion in Three-Dimensional Gödel Black Hole

2014 ◽  
Vol 2014 ◽  
pp. 1-9 ◽  
Author(s):  
J. Sadeghi ◽  
F. Pourasadollah ◽  
H. Vaez
Keyword(s):  
Black Hole ◽  
Brownian Motion ◽  
Angular Velocity ◽  
Heavy Quark ◽  
Brownian Particle ◽  
Three Dimensional ◽  
Btz Black Hole ◽  
Relativistic Limit ◽  
Black Hole Background ◽  
Gödel Black Hole

By using the AdS/CFT correspondence and Gödel black hole background, we study the dynamics of heavy quark under a rotating plasma. In that case we follow Atmaja (2013) about Brownian motion in BTZ black hole. In this paper we receive some new results for the case ofα2l2≠1. In this case, we must redefine the angular velocity of string fluctuation. We obtain the time evolution of displacement square and angular velocity and show that it behaves as a Brownian particle in non relativistic limit. In this plasma, it seems that relating the Brownian motion to physical observables is rather a difficult work. But our results match with Atmaja work in the limitα2l2→1.

scholarly journals Normal-mode analysis for scalar fields in BTZ black-hole background

2009 ◽  
Vol 60 (2) ◽  
pp. 169-173 ◽  
Author(s):  
Sayan K. Chakrabarti ◽  
Pulak Ranjan Giri ◽  
Kumar S. Gupta
Keyword(s):  
Black Hole ◽  
Normal Mode ◽  
Normal Mode Analysis ◽  
Scalar Fields ◽  
Mode Analysis ◽  
Btz Black Hole ◽  
Black Hole Background

Periodicity and area spectrum of the three dimensional BTZ black hole

2012 ◽  
Vol 44 (11) ◽  
pp. 2865-2872 ◽  
Author(s):  
Hui-Ling Li ◽  
Rong Lin ◽  
Li-Ying Cheng
Keyword(s):  
Black Hole ◽  
Three Dimensional ◽  
Area Spectrum ◽  
Btz Black Hole

Chiral modular bootstrap

2019 ◽  
Vol 34 (28) ◽  
pp. 1950168 ◽  
Author(s):  
M. Ashrafi
Keyword(s):  
Black Hole ◽  
Upper Bound ◽  
Three Dimensional ◽  
Conformal Weight ◽  
Two Dimensional ◽  
Btz Black Hole ◽  
Conformal Field ◽  
Dimensional Gravity ◽  
Large Spin ◽  
Dimension Ratio

Using modular bootstrap we show the lightest primary fields of a unitary compact two-dimensional conformal field theory (with [Formula: see text], [Formula: see text]) has a conformal weight [Formula: see text]. This implies that the upper bound on the dimension of the lightest primary fields depends on their spin. In particular if the set of lightest primary fields includes extremal or near extremal states whose spin to dimension ratio [Formula: see text], the corresponding dimension is [Formula: see text]. From AdS/CFT correspondence, we obtain an upper bound on the spectrum of black hole in three-dimensional gravity. Our results show that if the first primary fields have large spin, the corresponding three-dimensional gravity has extremal or near extremal BTZ black hole.

A Zeta Function for the BTZ Black Hole

2003 ◽  
Vol 18 (12) ◽  
pp. 2205-2209 ◽  
Author(s):  
F. L. Williams
Keyword(s):  
Black Hole ◽  
Zeta Function ◽  
Three Dimensional ◽  
Thermodynamic Quantities ◽  
Btz Black Hole ◽  
Special Values

For the three-dimensional BTZ black hole we consider a Selberg type zeta function. We indicate how special values of its logarithm correspond to certain thermodynamic quantities associated with the black hole.

scholarly journals Page curve for entanglement negativity through geometric evaporation

2022 ◽  
Vol 12 (1) ◽  
Author(s):  
Jaydeep Kumar Basak ◽  
Debarshi Basu ◽  
Vinay Malvimat ◽  
Himanshu Parihar ◽  
Gautam Sengupta
Keyword(s):  
Black Hole ◽  
Random Matrix Theory ◽  
Random Matrix ◽  
Mixed State ◽  
Dimensional Reduction ◽  
Matrix Theory ◽  
Three Dimensional ◽  
Two Dimensional ◽  
Btz Black Hole ◽  
Diagrammatic Technique

We compute the entanglement negativity for various pure and mixed state configurations in a bath coupled to an evaporating two dimensional non-extremal Jackiw-Teitelboim (JT) black hole obtained through the partial dimensional reduction of a three dimensional BTZ black hole. Our results exactly reproduce the analogues of the Page curve for the entanglement negativity which were recently determined through diagrammatic technique developed in the context of random matrix theory.

Brownian Motion of Rotating Particles

1968 ◽  
Vol 23 (4) ◽  
pp. 597-609 ◽  
Author(s):  
Siegfried Hess
Keyword(s):  
Brownian Motion ◽  
Angular Velocity ◽  
Brownian Particle ◽  
Planck Equation ◽  
Transverse Force ◽  
Particle Collision ◽  
Fokker Planck Equation ◽  
Rotational Motions ◽  
Transport Relaxation ◽  
Fokker Planck

A kinetic theory for the Brownian motion of spherical rotating particles is given starting from a generalized Fokker-Planck equation. The generalized Fokker-Planck collision operator is a sum of two ordinary Fokker-Planck differential operators in velocity and angular velocity space respectively plus a third term which provides a coupling of translational and rotational motions. This term stems from a transverse force proportional to the cross product of velocity and angular velocity of a Brownian particle. Collision brackets pertaining to the generalized Fokker-Planck operator are defined and their general properties are discussed. Application of WALDMANN'S moment method to the Fokker-Planck equation yields a set of coupled linear differential equations (transport-relaxation equations) for certain local mean values. The constitutive laws for diffusion, heat conduction by Brownian particles and spin diffusion are deduced from the transport-relaxation equations. The transport-relaxations coefficients appearing in them are given in terms of the two friction coefficients for the damping of translational and rotational motions and a third coefficient which is a measure of the transverse force. By the coupling of translational and rotational motions a diffusion flow gives rise to a correlation of linear and angular velocities.

scholarly journals Brownian motion of black holes in stellar systems with non-Maxwellian distribution of the field stars

2006 ◽  
Vol 2 (S238) ◽  
pp. 427-428
Author(s):  
Isabel Tamara Pedron ◽  
Carlos H. Coimbra-Araújo
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Distribution Function ◽  
Brownian Motion ◽  
Random Walk ◽  
Brownian Particle ◽  
Stellar System ◽  
Stellar Systems ◽  
Massive Black Hole ◽  
Nearby Stars

AbstractA massive black hole at the center of a dense stellar system, such as a globular cluster or a galactic nucleus, is subject to a random walk due gravitational encounters with nearby stars. It behaves as a Brownian particle, since it is much more massive than the surrounding stars and moves much more slowly than they do. If the distribution function for the stellar velocities is Maxwellian, there is a exact equipartition of kinetic energy between the black hole and the stars in the stationary state. However, if the distribution function deviates from a Maxwellian form, the strict equipartition cannot be achieved.The deviation from equipartition is quantified in this work by applying the Tsallis q-distribution for the stellar velocities in a q-isothermal stellar system and in a generalized King model.

scholarly journals STRING THEORY ON THREE-DIMENSIONAL BLACK HOLES

1998 ◽  
Vol 13 (08) ◽  
pp. 1229-1262 ◽  
Author(s):  
MAKOTO NATSUUME ◽  
YUJI SATOH
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
String Theory ◽  
Three Dimensional ◽  
Matching Condition ◽  
Target Space ◽  
Black Hole Mass ◽  
Curved Space ◽  
Conformal Field ◽  
Black Hole Background

We investigate the string theory on three-dimensional black holes discovered by Bañados, Teitelboim and Zanelli in the framework of conformal field theory. The model is described by an orbifold of the [Formula: see text] WZW model. The spectrum is analyzed by solving the level matching condition and we obtain winding modes. We then study the ghost problem and show explicit examples of physical states with negative norms. We discuss the tachyon propagation and the target space geometry, which are irrelevant to the details of the spectrum. we find a self-dual T-duality transformation reversing the black hole mass. We also discuss difficulties in string theory on curved space–time and possibilities of obtaining a sensible string theory on three-dimensional black holes. This work is the first attempt to quantize a string theory in a black hole background with an infinite number of propagating modes.

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