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Advances in High Energy Physics
Volume 2017 (2017), Article ID 3875746, 15 pages
Quantum Radiation Properties of General Nonstationary Black Hole
Department of Mathematics, Manipur University, Canchipur, Manipur 795003, India
Correspondence should be addressed to T. Ibungochouba Singh
Received 18 July 2016; Revised 30 November 2016; Accepted 4 January 2017; Published 5 March 2017
Academic Editor: Elias C. Vagenas
Copyright © 2017 T. Ibungochouba Singh. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP3.
Using the generalized tortoise coordinate transformations the quantum radiation properties of Klein-Gordon scalar particles, Maxwell’s electromagnetic field equations, and Dirac equations are investigated in general nonstationary black hole. The locations of the event horizon and the Hawking temperature depend on both time and angles. A new extra coupling effect is observed in the thermal radiation spectrum of Maxwell’s equations and Dirac equations which is absent in the thermal radiation spectrum of scalar particles. We also observe that the chemical potential derived from scalar particles is equal to the highest energy of the negative-energy state of the scalar particle in the nonthermal radiation in general nonstationary black hole. Applying generalized tortoise coordinate transformation a constant term is produced in the expression of thermal radiation in general nonstationary black hole. It indicates that generalized tortoise coordinate transformation is more accurate and reliable in the study of thermal radiation of black hole.
Hawking discovered the thermal radiation of black hole using the techniques of quantum field theory in curve space-time background and the derived radiation spectrum is purely thermal in nature [1, 2]. An important aspect in the study of black hole is to reveal the thermal and nonthermal radiation of black hole. References [3–5] have shown that the black hole has a nonzero finite entropy and the entropy of black hole is proportional to the horizon area. References [6, 7] also proposed the Hawking radiation as quantum tunneling process where the particles move in the dynamical geometry. They recovered a leading correction to the emission rate arising from the loss mass of the black hole. Following their works, Zhang and Zhao [8–10] have extended the method to more general circumstances for rotating black hole and they have shown the spectrum is no longer precisely thermal. Further, some information of the black hole can be obtained.
Akhmedov et al.  investigated the Hawking radiation as tunneling picture in the Schwarzschild black hole using the relativistic Hamilton-Jacobi method. The importance of this investigation is as follows: (i) if Schwarzschild coordinates or any other coordinates related to them via a transformation of spatial coordinates are used, we will get twice original Hawking temperature and (ii) any transformation involving time coordinates is utilized in the black hole evaporation, and it will give the original Hawking result. Following this method, many fruitful results have been obtained in [12–14]. This factor of two issues has been resolved via the discovery of the temporal contribution to the tunneling amplitude in the literatures [15–17]. The thermodynamics of black hole in lovelock gravity and in AdS space-time have been investigated by Cai [18–20]. One of the important aspects in this investigation is to calculate the Hawking temperature.
Recently, Angheben et al.  investigated Hawking radiation as tunneling of extremal and rotating black hole using the relativistic Hamilton-Jacobi method and WKB approximation without considering the particles backreaction. Since then many other authors applied the Hamilton-Jacobi method to study the Hawking radiation for more general space-time [22–25]. Choosing appropriate Gamma matrices, the Hawking radiation as tunneling from Dirac particles was investigated in  for the general stationary black hole. By inserting the wave function into the Dirac field equations, the action of the radiant particles is derived. This result is related to the Boltzmann factor of emission at the Hawking radiation temperature in accordance with semiclassical WKB approximation. References [27, 28] introduced tortoise coordinate transformation to study the Hawking radiation of black hole in which gravitational field is independent of time. Using tortoise coordinate transformation, Klein-Gordon equation, Maxwell’s electromagnetic field equations, and Dirac particles can be transformed into single form of wave equation near the event horizon. Separating the variables from the standard wave equation, ingoing wave and outgoing wave can be obtained. Extending the wave equation from outside the event horizon into the inside by rotating through the lower half of the complex plane, the thermal radiation spectra can be derived. Generalizing this method, many more works have been done [29–31].
References [32, 33] have also investigated the Hawking radiation by calculating the vacuum expectation values of the renormalized energy momentum tensor of spherically symmetric nonstationary black hole. These results are consistent with [27, 28]. However all these research works were confined to the quantum thermal radiation of black hole only. In addition to the quantum thermal radiation, the importance of quantum nonthermal radiation of black hole has been studied by different authors in different types of space-time in the literatures [34–38].
The main aim of this paper is to investigate thermal radiation from Klein-Gordon equation, Maxwell’s electromagnetic field equations, Dirac particles, and also nonthermal radiation of Hamilton-Jacobi equation in general nonstationary black hole. It gives the relationship between two kinds of radiation in the case of scalar particles. A new extra coupling effect is derived from the thermal radiation spectrum of Maxwell’s field equations and Dirac particles. In Section 2, we derive the location of horizon in general nonstationary black hole using null surface condition and generalized tortoise coordinate transformation. In Section 3, adjusting the parameter , the Klein-Gordon equation is transformed into a wave equation near the event horizon in general nonstationary black hole. In Section 4, we derive asymptotic behaviors of first-order form of four equations and second-order form of three equations from the Maxwell’s electromagnetic field equations near the event horizon using generalized tortoise coordinate transformation (GTCT). In Section 5, the asymptotic behaviors of the first-order form of four equations and second-order form of two equations are deduced from the Dirac particles using the GTCT near the event horizon. In Section 6, the second-order form of Klein-Gordon equation, the three second-order forms of Maxwell’s equations, and the two second-order forms of Dirac equations are transformed into single standard form of equation near the black hole event horizon. By separating the wave equation the chemical potential and the thermal radiation spectra can be obtained. In Section 7, the highest energy of nonthermal radiation is obtained from the relativistic Hamilton-Jacobi equation. In Section 8, we derive the expression of a new extra coupling effect which is absent from the thermal radiation spectrum of scalars particles. The relationship between thermal and nonthermal radiation in general nonstationary black hole is also established. Some conclusions are given in the last section.
2. General Nonstationary Black Hole
The line element describing the most general nonstationary black hole is given bywhere we assume the retarded Eddington-Finkelstein coordinates , and and make the conventions that all indices of Greek letters and all indices of Latin letters . The event horizon in general nonstationary black hole can be characterized by null hypersurface condition: . The null hypersurface condition gives the position of horizon of stationary or nonstationary black hole The location and the temperature of the horizon in a nonstationary black hole may be obtained by applying tortoise coordinate transformation. By using tortoise coordinate transformation of the form , the Klein-Gordon equation, the Maxwell’s electromagnetic field equations, and the Dirac particles can be combined into a standard form of wave equation in a nonstationary or stationary space-time (where is the surface gravity). The location of horizon may be assumed as functions of retarded time coordinate and different angles . The space-time geometry outside the event horizon is described by tortoise coordinate only and, in this condition, approaches to positive infinity when tending to infinite point and tends to negative infinity at the event horizon. It is also assumed that the geometry of space-time in the general nonstationary black hole is symmetric about -axis. According to [40–46], the generalized tortoise coordinate transformation is defined aswhere , , and are the parameters under the tortoise coordinate transformation. From (3), we getUsing (4) in (2), the horizon equation in general nonstationary black hole is obtained aswhere . represents the evaporation rate in general nonstationary black hole near the event horizon. The event horizon is expanded gradually if (absorbing black hole), where, as , the event horizon is contracted. In addition, and denote the rate of event horizon varying with angles and also describe the rotation effect of nonstationary black hole. is the location of event horizon and depends on retarded time and angular coordinates , and also is an adjustable parameter that depends on retarded time and angular coordinates.
3. Klein-Gordon Equation
In this section, the asymptotic behavior of minimally electromagnetic coupling Klein-Gordon equation near the black hole will be discussed. The Klein-Gordon equation describes the explicit form of wave equation of the scalar particles with mass in curve space-time which is given byUsing generalized tortoise coordinate transformation to (6) and subsequently multiplying by the factor to both sides of (6) and finally taking limit near the event horizon as , , , and , the second-order form of wave equation is obtained as follows:whereBy adjusting parameter , the coefficient of is assumed to be unity near the event horizon, and we getIt is also observed that, in the left hand side of (9), both numerator and denominator tend to zero near the event horizon . Hence (9) is an indeterminate form of . Using L’Hospital rule and using (5), the surface gravity is obtained from the Klein-Gordon scalar particles as follows:
4. Maxwell’s Electromagnetic Field Equations
To write the explicit form of Maxwell’s electromagnetic field equations in Newman-Penrose formalism , the following complex null tetrad vectors , , , and are chosen at each point in four-dimensional space, where and are a pair of real null tetrad vectors and and are a pair of complex null tetrad vectors. They are required to satisfy the following conditions:and corresponding directional derivatives are given byThe dynamical behavior of spin-1 particles in curve space-time is given by four coupled Maxwell’s electromagnetic field equations expressed in Newman-Penrose formalism  as follows:where , , and are the four components of Maxwell’s spinor in the Newman-Penrose formalism. , and are spin coefficients introduced by Newman and Penrose, and they are given bywhere , , , , , , , and are complex conjugates of , , , , , , , and . From (13), the three second-order forms of Maxwell’s equations for (, , ) components are given byReferences [49, 50] have shown that (13) cannot be decoupled except only for the stationary black hole space-time. For studying the thermal radiation in general nonstationary black hole, the asymptotic behavior of the first-order and second-order form of (13) near the event horizon will be considered. Then, after taking the limit as , , , and , the first-order forms of Maxwell’s equations near the event horizon are as follows:We assume that the three derivatives , , and in (18) are nonzero. Then nontrivial solutions for , , and can be obtained if the determinant of their coefficients is zero, which will give the horizon equation like the null surface condition (5). The importance of (18) is to eliminate the crossing terms involved in the second-order form of Maxwell’s equations near the event horizon.
Utilizing the generalized coordinate transformation (3) to (15), (16), and (17) and subsequently multiplying by the factor to both sides of three second-order equations for the coefficients , , and to be and finally taking the limit of , , , and , then the three second-order forms of Maxwell’s electromagnetic field equations near the event horizon can be expressed as follows:wherewherewhereWe assume the value of approaches unity near the event horizon, and then we getwhich is an indeterminate form of and, applying L’Hospital rule, the surface gravity due to the Dirac particles is given bywhich is equal to the surface gravity derived from Klein-Gordon scalar particle given by (10).
5. Dirac Equations
The four couples of Dirac equations  expressed in Newman-Penrose formalism are given by where , , , and are the directional derivatives given by (12) and , and are spin coefficients and also is the mass of the Dirac particles. , and are the four components of Dirac spinor in the Newman-Penrose formalism. Equations (27) can be decoupled only for the stationary black hole space-time. From (27) the second-order forms of Dirac equations for the components are given byApplying generalized tortoise coordinate transformation to (27), after taking limit , , , and , the first-order forms of Dirac equations near the event horizon are given byIn order to study Hawking thermal radiation from Dirac particles, we should consider the asymptotic behavior of (27) near the black hole horizon. The nontrivial solutions for , , , and can be obtained if the four derivatives , , , and in (30) are nonzero. Equations (30) may be used to eliminate the crossing terms that appeared in the second-order form of Dirac equation near the horizon.
Applying generalized tortoise coordinate transformation to (28) and (29), via some arrangement, and multiplying by the factor to both sides of the two second-order forms of Dirac equations for the coefficients and to be 2 and taking the limit of , , , and , the two second-order forms of Dirac equations can be written as follows:wherewhereand when approaches unity, we obtainEquation (35) is a indeterminate form. By applying L’Hospital rule near the black hole event horizon, the surface gravity due to Dirac particle is given by which is the same as (10) and (26), the surface gravities derived from Klein-Gordon scalar particles, and Maxwell’s electromagnetic field equations.
6. Thermal Radiation Spectrum
To investigate the thermal radiation spectrum in general nonstationary black hole, we combine the second-order form of Klein-Gordon equation (7), the three second-order forms Maxwell’s equations (19), (21), and (23), and the two second-order forms of Dirac equations (31) and (33) as single form of wave equation near the event horizon as follows:whereEquation (37) may be assumed as standard form of wave equation in general nonstationary black hole near the horizon . It includes Klein-Gordon equation, Maxwell’s electromagnetic field equations, and Dirac equations with different coefficient of constant terms.
For example, when for the Klein-Gordon equation, (37) gives the following constants:
For Maxwell’s electromagnetic equations , the constant terms areFor Lastly, for , we getSimilarly for Dirac particles when , (37) gives the following constant terms:and, for , we obtainEquation (37) may be assumed as second-order partial differential equation near the event horizon in general nonstationary black hole since all the coefficients , , , and are constant terms when , , , and .
Using [29, 30, 36, 52], the variables in (37) may be separated for the analysis of the field equations aswhere is an arbitrary real function and is the energy of the particles which depend on tortoise coordinate transformation; and are components of generalized momentum of scalar particles. And we use and , where is Hamiltonian function of scalar particles. Using (45) into (37) and after separating the variables, the radial and angular parts are given bywhere and are a constant and function of retarded time in variable of separation, respectively, where and .
After separation of variables, the radial components of two independent solutions are defined bywhere represents an incoming wave which is analytic at ; denotes an outgoing wave having singularity at the event horizon. References [27, 28] indicate that can continue analytically from outside of the event horizon into inside by rotating through lower half of the complex plane asFrom (47) and (48), one can obtain the relative scattering probability near the event horizon :whereFollowing Damour and Ruffini  and extended by Sannan , the thermal radiation spectrum of Maxwell’s electromagnetic field equations (Dirac particles or scalar particles) from general nonstationary black holes is given bywhere is Boltzmann constant and upper positive symbol stands for the Fermi-Dirac distribution and the lower negative symbol corresponds to the Bose-Einstein statistics, showing that black hole radiates like a black body radiation. The Hawking temperature is given byand the chemical potential is given byIntegrating the thermal radiation spectra (51) or distribution function over all ’s the combined form of Hawking flux for Klein-Gordon scalar particles, Maxwell’s electromagnetic field equations, and Dirac equations can be obtained as follows:This is an exact result for the energy flux in general nonstationary black hole. If in (54), the Hawking flux for fermions is given byand the Hawking flux for boson is defined byThese results are consistent with ones already obtained in the literature [53, 54]. From (52), we observe that is a function of retarded time and different angles. Hence, it is a distribution of temperature of the thermal radiation near the event horizon due to the Klein-Gordon scalar field, the Maxwell’s electromagnetic field equations, and the Dirac equations in general nonstationary black hole. It has been shown that the constant coefficient appears in the expression of chemical potential and may represent a particular energy term for Maxwell’s electromagnetic field and Dirac particles which is absent in the thermal radiation spectrum of other scalar particles.
7. Nonthermal Radiation
The relativistic Hamilton-Jacobi equation for the classical action of a particle of mass in a curve space-time is given by where is the Hamiltonian principal function. Using (3) into (57), we obtain the following:whereMultiplying by the factor to both sides of (58) and assuming the resulting coefficient of