Hawking radiation from the charged and magnetized BTZ black hole via covariant anomaly

This paper discusses Hawking radiation from the charged and magnetized Bafiados-Teitelboim-Zanelli （BTZ） black hole from the viewpoint of anomaly, initiated by Robinson and Wilczek recently. It reconstructs the electromagnetic field tensor and the Lagrangian of the field corresponding to the source with electric and magnetic charges to redefine an equivalent charge and gauge potential. It employs the covariant anomaly cancellation method to determine the compensating fluxes of charge flow and energy-momentum tensor, which are shown to match with those of the 2- dimensional blackbody radiation at the Hawking temperature exactly.

P-V Criticality of a Modified BTZ Black Hole in 2 + 1 Dimensional Intrinsic Time Quantum Gravity

Intrinsic time quantum geometrodynamics is a formulation of quantum gravity naturally adapted to 3 + 1 dimensions. In this paper we construct its analogous 2 + 1 formulation, taking note of the mathematical structures which are preserved. We apply the resulting construction to convert the BTZ black hole metric to ITQG framework. We then modify the BTZ black hole in order to investigate the existence of the P-V criticality in ITQG theory.

An optical analogue for rotating BTZ black holes

We demonstrate an optical realization for the rotating BTZ black hole using the recent popular photon fluid model in an optical vortex but with a new proposed expression for the optical phase.We also give the numerical realization for the optical vortex to ensure that it can be generated experimentally.Different from the earlier suggestions for the analogue rotating black holes,our proposal includes an inner horizon in the analogue black hole structure.Such structure can keep for a long distance for the convenience of observing analogue Hawking or Penrose radiations.

Area spectra of BTZ black holes via periodicity

Motivated by the recent work that the periodicity of a black hole is responsible for the area spectrum,we exclusively utilize the period of motion of an outgoing wave,which is shown to be related to the vibrational frequency of the perturbed black hole,to study area spectra of a non-rotating BTZ black hole and a rotating BTZ black hole.It is found that the area spectra and entropy spectra for both space times are equally spaced.In addition,we find that though the entropy spectra of the 3-dimensional BTZ black holes take the same form as those of the 4-dimensional black holes,the area spectra depend on the dimension of space times.Our result confirms that the entropy spectrum of a black hole is more fundamental than the area spectrum.

Spectroscopy of the rotating BTZ black hole via adiabatic invariance

According to Bohr-Sommerfeld quantization rule,an equally spaced horizon area spectrum of a static,spherically symmetric black hole was obtained under an adiabatic invariant action.This method can be extended to the rotating black holes.As an example,this method is applied to the rotating BTZ black hole and the quantized spectrum of the horizon area is obtained.It is shown that the area spectrum of the rotating BTZ black hole is also equally spaced and irrelevant to the rotating parameter,which is consistent with the Bekenstein conjecture.Specifically,the derivation does not need the quasinormal frequencies and the small angular momentum limit.

Conformal field theory on the horizon of a BTZ black hole

In a three-dimensional spacetime with ~egative cosmological constant, general relativity can be written as two copies of SO（2,1） Chern-Simons theory. On a manifold with a boundary, the Chern-Simons theory induces a conformal field theory——Wess-Zumino-Witten theory on the boundary. In this paper, it is shown that with suitable boundary conditions for a Banados-Teitelboim-Zanelli black hole, the Wess-Zumino-Witten theory can reduce to a chiral massless scalar field on the horizon.

Scalar field in massive BTZ black hole and entanglement entropy

In this paper,we investigate the quantum scalar fields in a massive BTZ black hole background.We study the entropy of the system by evaluating the entanglement entropy using a discretized approach.Specifically,we fit the results with a log-modified formula of the black hole entropy,which is introduced by quantum correction.The coefficients of leading and sub-leading terms affected by the mass of graviton are numerically analyzed.

Collision of spinning particles near BTZ black holes

We study the collision property of spinning particles near a Banados-Teitelboim-Zanelli(BTZ)black hole.Our results show that although the center-of-mass energy of two ingoing particles diverges if one of the particles possesses a critical angular momentum,the particle with critical angular momentum cannot exist outside of the horizon due to violation of the timelike constraint.Further detailed investigation indicates that only a particle with a subcritical angular momentum is allowed to exist near an extremal rotating BTZ black hole,and the corresponding collision center-of-mass energy can be arbitrarily large in a critical angular momentum limit.

Entropy of three-dimensional BTZ black holes

The entropies of scalar field and neutrino field are calculated in the background of three-dimensional BTZ black hole. Considering statistical physics,we propose not to consider the superraradiant modes for bosons (Fermion fields do not display supperradiance).In fact,the nonsuperradiant modes do contribute exactly the area entropy for both bosons and fermions. The result shows that the neutrino field entropy is 3/2 times the scalar one.

Thermodynamics and weak cosmic censorship conjecture of BTZ black holes in extended phase space

As a charged fermion drops into a BTZ black hole, the laws of thermodynamics and the weak cosmic censorship conjecture are investigated in both the normal and extended phase space, where the cosmological parameter and renormalization length are regarded as extensive quantities. In the normal phase space, the first and second law of thermodynamics, and the weak cosmic censorship are found to be valid. In the extended phase space, although the first law and weak cosmic censorship conjecture remain valid, the second law is dependent on the variation of the renormalization energy dK. Moreover, in the extended phase space, the configurations of extremal and near-extremal black holes are not changed, as they are stable, while in the normal phase space, the extremal and near-extremal black holes evolve into non-extremal black holes.

Spectroscopy via adiabatic covariant action for the Baados-Teitelboim-Zanelli (BTZ) black hole

Very recently, via the covariant form of the adiabatic invariant I = ∮pidqi instead of I = ∮pidqi, an equally spaced spectroscopy of a Schwarzschild black hole was derived. The emphasis was given to the covariant of results. In this paper, we extend that work in a spherically symmetric spacetime to the case of a rotating Bafiados-Teitelboim-Zanelli （BTZ） black hole. It is noteworthy that the adiabatic covariant action I = ∮pidqi gives the same value for the black hole spectroscopy in different coordinates. The result shows that the area spectrum is △A = 8πl2p, which confirms Bekenstein＇s initial proposal. And the result is consistent with that already obtained by other methods.

带电BTZ黑洞一般性辐射的隧穿效应

研究了BTZ黑洞背景下带电、有质量粒子的辐射过程,此时能量守恒和电荷守恒意味着引力反作用和电磁反作用.从隧穿过程的观点来看,辐射谱偏离了纯热谱,但仍满足幺正理论,并且有可能对信息佯谬给出解释.通过计算,可以得到与不带电、无质量粒子辐射相同的结论.

BTZ Quasinormal Frequencies as Poles of Green’s Function

Based on the well known fact that the quasinormal frequencies are the poles of the frequency domain Green’s function we describe a method that allows us to calculate exactly the quasinormal frequencies of the Klein-Gordon field moving in the three-dimensional rotating Bañados-Teitelboim-Zanelli black hole. These quasinormal frequencies are already published and widely explored in several applications, but we use this example to expound the proposed method of computation. We think that the described procedure can be useful to calculate exactly the quasinormal frequencies of classical fields propagating in other backgrounds. Furthermore, we compare with previous results and discuss some related facts.

荷电旋转BTZ黑洞的Hawking隧穿辐射

运用Parikh量子隧穿模型,研究荷电旋转BTZ黑洞的量子隧穿效应.其结果表明:在能量守恒和角动量守恒的条件下,黑洞视界处的粒子出射率与熵变有关,辐射谱不再是严格的纯热谱.

Microscopic states of Kerr black holes from boundary-bulk correspondence

It was previously claimed by the author that black holes can be considered as topological insulators. Both black holes and topological insulators have boundary modes, and the boundary modes can be described by an effective BF theory. In this paper, the boundary modes on the horizons of black holes are analyzed using methods developed for topological insulators. BTZ black holes are analyzed first, and the results are found to be compatible with previous works. The results are then generalized to Kerr black holes, for which new results are obtained: dimensionless right-and left-temperatures can be defined and have well behavior in both the Schwarzschild limit a → 0 and the extremal limit a → M. Upon the Kerr/CFT correspondence, a central charge c = 12 Mr+ can be associated with an arbitrary Kerr black hole. Moreover, the microstates of the Kerr black hole can be identified with the quantum states of this scalar field. From this identification, the number of microstates of the Kerr black hole can be counted, yielding the Bekenstein-Hawking area law for the entropy.

W-hairs of the black holes in three-dimensional spacetime

In a previous publication,we claimed that a black hole can be considered as a topological insulator.A direct consequence of this claim is that their symmetries should be related.In this paper,we give a representation of the near-horizon symmetry algebra of the BTZ black hole using the W1+∞symmetry algebra of the topological insulator in three-dimensional spacetime.Based on the W1+∞algebra,we count the number of the microstates of the BTZ black holes and obtain the Bekenstein-Hawking entropy.

广义测不准关系与三维BTZ黑洞熵

通过应用在量子引力中,由广义测不准关系得出的新的态密度方程,研究三维BTZ背景下黑洞的熵.当取广义测不准关系中引入的,具有Planck量级与空间维数有关的常数λ为特定值时,得到BTZ黑洞Bekenstein-Hawking熵和修正项.由于利用新的态密度方程,在计算中不存在用brick-wall模型计算黑洞熵时出现的发散项和小质量近似.所得结论,从量子统计力学角度给出了黑洞Bekenstein-Hawking熵的修正值,使人们对黑洞熵的修正值有更深入的认识.