Recently the modified Dirac equation with Lorentz invariance violation has been proposed, which would be helpful to resolve some issues in quantum gravity theory and high energy physics. In this paper, the modified Dirac equation has been generalized in curved spacetime, and then fermion tunneling of black holes is researched under this correctional Dirac field theory. We also use semiclassical approximation method to get correctional Hamilton-Jacobi equation, so that the correctional Hawking temperature and correctional black hole’s entropy are derived.
Fundação de Amparo à Pesquisa do Estado de São Paulo2012/08934-0Conselho Nacional de Desenvolvimento Científico e TecnológicoCoordenação de Aperfeiçoamento de Pessoal de Nível SuperiorNational Natural Science Foundation of China115730221120525411178018113752791. Introduction
In 1974, Hawking proved black holes could radiate Hawking radiation once considering the quantum effect near the horizons of black holes [1, 2]. This theory indicates that black hole would be viewed as thermodynamic system, so that black hole physics can be connected closely with gravity, quantum theory, and thermodynamics physics. According to the view point of quantum tunneling theory, the virtual particles inside of black hole could cross the horizon due to the quantum tunneling effect and become real particles and then could be observed by observers as Hawking radiation. Wilczek et al. proposed a semiclassical method to study the quantum tunneling from the horizon of black hole [3–21]. Along with this method, the Hamilton-Jacobi method was applied to calculate the Hawking tunneling radiation. According to the Hamilton-Jacobi method, the wave function of Klein-Gordon equation can be rewritten as Φ=CexpiS/ħ (where S is semiclassical action) and Hamilton-Jacobi equation is obtained via semiclassical approximation. Using the Hamilton-Jacobi equation, the tunneling rate could be calculated by the relationship Γ~exp-2ImS (where Γ is the tunneling rate at the horizon of black hole), and then the Hawking temperature can be determined. People have applied this method to research Hawking tunneling radiation of several static, stationary, and dynamical black holes.
However, since the Hamilton-Jacobi equation is derived from Klein-Gordon equation, original Hamilton-Jacobi method just can be valid for scalar particles in principle. Therefore, Kerner and Mann studied fermions tunneling of black hole by a new method [22–32], which assumes the wave function of Dirac equation Ψ as spin-up and spin-down and then calculates the fermions tunneling, respectively. Nevertheless, this method is still impossible to apply in arbitrary dimensional spacetime. Our work in 2009 showed that the Hamilton-Jacobi equation can also be derived from Dirac equation via semiclassical approximation, so we proved that the Hamilton-Jacobi equation can be used to study the fermions tunneling directly [33–35].
On the other hand, as the basis of general relativity and quantum field theory, Lorentz invariance is proposed to be spontaneously violated at higher energy scales. A possible deformed dispersion relation is given by [36–44] (1)p02=p→2+m2-Lp0αp→2,where p0 and p→ are the energy and momentum of particle and L is “minimal length” with the order of the Plank length. The work of spacetime foam Liouville string models has introduced this relation with α=1, and people also proposed quantum equation of spineless particles by using this relation. Recently, Kruglov considers the deformed dispersion relation with α=2 and proposes modified Dirac equation [45]: (2)γ¯μ∂μ+m-iLγ¯t∂tγ¯j∂jψ=0,where γ¯a is ordinary gamma matrix and j is space coordinate, while μ is spacetime coordinate. The effect of the correctional term would be observed in higher energy experiment.
In this paper, we try to generalize the modified Dirac equation in curved spacetime and then study the correction of Hawking tunneling radiation. In Section 2, the modified Dirac equation in curved spacetime is constructed and then the modified Hamilton-Jacobi equation is derived via semiclassical approximation. We apply the modified Hamilton-Jacobi equation to the fermions tunneling radiation of 2+1-dimensional black string and higher dimensional BTZ-like black strings in Sections 3 and 4, respectively, and Section 5 includes some conclusion and the discussion about the correction of black hole’s entropy.
2. Modified Dirac Equation and Hamilton-Jacobi Equation in Curved Spacetime
As we all know, the gamma matrix and partial derivative should become gamma matrix in curved spacetime γa and covariant Da derivative, respectively, namely,(3)γ¯a⟶γa,∂a⟶Da=∂a+Ωa+iħeAa,where γa satisfy the relationship γa,γb=γaγb+γbγa=2gabI, eAa is charged term of Dirac equation, and Ωμ=(1/8)γaγb-γbγaeaν∂μebν-Γμνcebc is spin connection. According to this transformation, we can construct the modified Dirac equation in curved spacetime as (4)γμDμ+mħ-σħγtDtγjDjΨ=0,where we choose c=1 but ħ≠1, while c=ħ=1 in (1) and (2). It is assumed that σ≪1, so that the correctional term σħγtDtγjDj is very small.
Now let us use the modified Dirac equation to derive the modified Hamilton-Jacobi equation. Firstly, we rewrite the wave function of Dirac equation as [33–35] (5)Ψ=ζt,xjexpiħSt,xj,where ζt,xj and Ψ are m×1 matrices and ∂tS=-ω. In semiclassical approximation, we can consider that ħ is very small, so that we can neglect the terms with ħ after dividing by the exponential terms and multiplying by ħ. Therefore, (4) is rewritten as (6)iγμ∂μS+eAμ+m-σγtω-eAtγj∂jS+eAjζt,xj=0.Considering the relationship (7)γμ∂μS+eAμ=-γtω-eAt+γj∂jS+eAj,we can get (8)iΓμ∂μS+eAμ+Mζt,xj=0,where(9)Γμ=1+iσω-eAtγtγμ,M=m-σgttω-eAt2.Now, multiplying both sides of (9) by the matrix -iΓν∂νS+eAν, we can obtain (10)Γν∂νS+eAνΓμ∂μS+eAμζ-iMΓν∂νS+eAνζ=0.The second term of the above equation could be simplified again by (8), so the above equation can be rewritten as (11)ΓνΓμ∂νS+eAν∂μS+eAμζ+M2ζ=0,where we can prove the relation (12)ΓνΓμ=γνγμ+2iσω-eAtgtνγμ+Oσ2.We always ignore O(σ2) terms because σ is very small. Now, let us exchange the position of μ and ν in (11) and consider the relation of gamma matrices γa,γb=2gabI; then we can obtain (13)γαγβ+γαγβ2∂αS+eAα∂βS+eAβ+m2-2σmgttω-eAt2+2iσω-eAtgtρ∂ρS+eAργμ∂μS+eAμζ+Oσ2=gαβ∂αS+eAα∂βS+eAβ+m2-2σmgttω-eAt2+2iσω-eAtgtρ∂ρS+eAργμ∂μS+eAμζ+Oσ2=0.Namely,(14)iσγμ∂μS+eAμ+Mζt,xj=0,where(15)M=gαβ∂αS+eAα∂βS+eAβ+m2-2σmgttω-eAt22gtρ∂ρS+eAρω-eAt.Using the idea of (10)-(11) again, we can multiply both sides of (15) by the matrix -iγν∂νS+eAν, so that the equation becomes (16)σγν∂νS+eAνγμ∂μS+eAμζ-iMγν∂νS+eAνζ=0.The second term of the above equation could be simplified again by (15). Then, exchange μ and ν and use the relationship γa,γb=2gabI, so the above equation can be rewritten as (17)γνγμ+γμγν2σ2∂νS+eAν∂μS+eAμ+M2ζt,xj=σ2gμν∂νS+eAν∂μS+eAμ+M2ζt,xj=0.The condition that (17) has nontrivial solution required the determinant of coefficient in (17) should vanish, so we can directly get the equation (18)σ2gμν∂νS+eAν∂μS+eAμ+M2=0.Consider the square root for left side of (18) and ignore all Oσ2 terms, so we can directly get the modified Hamilton-Jacobi equation: (19)gμν∂νS+eAν∂μS+eAμ+m2-2σmgttω-eAt2=0.
Therefore, we find that the modified Dirac equation from Lorentz invariance violation could lead to the modified Hamilton-Jacobi equation, and the correction of Hamilton-Jacobi equation depends on the energy and mass of radiation fermions. Using the modified Hamilton-Jacobi equation, we then investigate the fermions Hawking tunneling radiation of 2+1-dimensional black string and n+1-dimensional BTZ-like string in the following two sections.
3. Fermions Tunneling of 2+1-Dimensional Black String
The research of gravity in 2+1 dimension can help people further understand the properties of gravity, and it is also important to construct the quantum gravity. Recently, Murata et al. have researched the 2+1-dimensional gravity with dilaton field, whose action is given by [46] (20)I=M3∫d3x-gBR+λ2B,where B, M3, and λ are, respectively, the dilaton field, 3-dimensional Planck mass, and the parameter with mass dimension. The static black string solution is given by(21)ds2=-lnrrHdt2+lnrrH-1dr2+dy2,B=λr.It is evident that the horizon of this black hole is rH, but the black string is unstable as rH≲L (where L is scale of compactification), so it is assumed that rH≫L.
Now we research the fermions tunneling of this black hole, so the modified Hamilton-Jacobi equation in this spacetime is given by (22)-1-2σmlnrrH-1ω2+lnrrHdRdr2+dYdy2+m2=0,where we have set S=-ωt+R(r)+Y(y), yielding the radial Hamilton-Jacobi equation as (23)-1-2σmlnrrH-1ω2+lnrrHdRdr2+λ0+m2=0,where the constant λ0 is from separation of variables, and (23) finally can be written as (24)R±r=±∫lnrrH-11-2σmω2-lnrrHλ0+m2.At the horizon rH of the black string, the above equation is integrated via residue theorem, and we can get (25)R±r=±iπ1-σmrHωand the fermions tunneling rate (26)Γ=exp-2ħImS=exp-2ħImR+-ImR-=e-4π/ħ1-σmrHω=e-ω/TH.The relationship between tunneling rate and Hawking temperature required (27)TH=ħ1+σm4πrH=1+σmT0,where TH and T0 are the modified and nonmodified Hawking temperature of the 2+1-dimensional black string, respectively, and σ term is the correction.
4. Fermions Tunneling of Higher Dimensional BTZ-Like Black Strings
As we all know that the linear Maxwell action fails to satisfy the conformal symmetry in higher dimensional spacetime [47, 48], so Hassaïne and Martínez proposed gravity theory with nonlinear Maxwell field in arbitrary dimensional spacetime:(28)I=-116π∫Mdn+1x-gR+2l2-βαFμνFμνs,where Λ≡-l-2 is cosmological constant. Hendi researched n+1-dimensional static black strings solution with β=1, α=-1, and s=n/2, and it is charged BTZ-like solutions [49], whose metric is (29)ds2=-frdt2+dr2fr+r2∑kdxk2,where(30)fr=r2l2-r2-nM+2n/2Qn-1At,and the electromagnetic potential is (31)A=Atdt=Qlnrldt.As n=2, this solution is no other than the static charged BTZ solution. We will study the Hawking radiation and black hole temperature at the event horizon rH of this black string. In (19), we can set S=-ωt+R(r)+Y(xk), where xk are the space coordinates excluding the radial coordinate, so that the modified Hamilton-Jacobi equation is given by (32)-1-2σmf-1rω-eAt2+frdRdr2+1r2∑kdYdxk2+m2=0,and the radial equation with constant λ0 is (33)-1-2σmf-1rω-eAt2+frdRdr2+λ0r2+m2=0.Therefore, at the horizon rH of the black string, f(rH)=0 and we finally get (34)R±r=±∫fr-11-2σmω-eAt2-frλ0+m2=±iπ1-σmω-ω0f′rH,where ω0=eAt(rH). This means that the fermions tunneling rate is (35)Γ=exp-2ħImS=exp-2ħImR+-ImR-=e-4π/ħ1-σmω-ω0/f′rH=e-ω-ω0/THand the Hawking temperature is (36)TH=ħ1+σm4πf′rH=ħ1+σm4πnrHl2-2n/2QnrH1-n=1+σmT0,where TH and T0 are the modified and nonmodified Hawking temperature of the n+1-dimensional BTZ-like black string, respectively, and σ term is the correction.
5. Conclusions
In this paper, we consider the deformed dispersion relation with Lorentz invariance violation and generalize the modified Dirac equation in curved spacetime. The fermions tunneling radiation of black strings is researched, and we find that the modified Dirac equation could lead to Hawking temperature’s correction, which depends on the correction parameter σ and particle mass m in the modified Dirac equation. Next we will discuss the correction of black hole entropy in this theory.
The first law of black hole thermodynamics requires (37)dM=TdS+ΞdJ+UdQ,where Ξ and U are electromagnetic potential and rotating potential, so the nonmodified entropy of black hole is [1, 2, 50, 51] (38)dS0=dM-ΞdJ-UdQT0.From the above results, we know that the relationship between modified and nonmodified Hawking temperature is TH=(1+σm)T0, since the nonmodified black hole entropy is given by (39)SH=∫dSH=∫dM-ΞdJ-UdQ1+σmT0=S0-m∫σdS0+Oσ2,where we can ignore O(σ2) because σ≪1. Equation (39) shows that the correction of black hole entropy depends on σ, which is independent from time and space coordinates. However, it is possible that σ depends on other parameters in curved spacetime, and it is very interesting that σ depends on S0. In particular, as σ=σ0/S0+⋯, we can get the logarithmic correction of black hole entropy (40)SH=S0-mσ0lnS0+⋯.In quantum gravity theory, the logarithmic correction has been researched in detail [52–69], and according to [70], it is required that the coefficient of logarithmic correction should be -(n+1)/2(n-1) in n+1-dimensional spacetime, so it indicates that σ0 could be (n+1)/2m(n-1).
On the other hand, from the deformed dispersion relation (1) with α=2, it is implied that the Klein-Gordon equation could be given by (41)-∂t2+∂j2+m2-σ2ħ2∂t2∂j2Φ=0,so the generalized uncharged Klein-Gordon equation in static curved spacetime is (42)gtt∇t2+gjj∇j2+m2+σ2ħ2gtt∇t2gjj∇j2Φ=0,and using the semiclassical approximation with Φ=CexpiS/ħ, the modified Hamilton-Jacobi equation in scalar field is given by (43)1+σ2gttω2gμν∂μS∂νS+m2-σ2gtt2ω4=0.Namely, (44)gμν∂μS∂νS+m2-σ2gttω2m2+gttω2+Oσ4=0.Contrasting (19) and (44) as uncharged case, we find that the correctional terms of Dirac field and scalar field are very different. The fact implies that the corrections of Hawking temperature and black hole entropy from Hawking tunneling radiation with different spin particles could be different, and this conclusion could be helpful to suggest a new idea to research the black hole information paradox. Work in these fields is currently in progress.
Competing Interests
The authors declare that they have no competing interests.
Acknowledgments
This work was supported by FAPESP no. 2012/08934-0, CNPq, CAPES, and National Natural Science Foundation of China no. 11573022, no. 11205254, no. 11178018, and no. 11375279.
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