# Covariant GUP Deformed Hamilton-Jacobi Method

Authors: Benrong Mu; Peng Wang; Haitang Yang
Journal: Advances in High Energy Physics
 (2017)

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## Abstract

We first briefly revisit the original Hamilton-Jacobi method and show that the Hamilton-Jacobi equation for the actionI of tunneling of a fermionic particle from a charged black hole can be written in the same form of that for a scalar particle. On the other hand, various theories of quantum gravity suggest the existence of a minimal length scale, incorporating of which into quantum mechanics implies a modification of the uncertainty principle. In the scenario incorporating the generalized uncertainty principle (GUP) into a quantum field theory (QFT) in a covariant way, we derive the deformed model-independent KG/Dirac and Hamilton-Jacobi equations using the methods of effective field theory. For this Lorentz invariant GUP modified QFT, we find that the effect of GUP on the Hamilton-Jacobi equations is simply to “renormalize” the mass of the emitted particles, from m to meff. Therefore, in this scenario, the Hawking temperature of a black hole does not receive any corrections from the GUP effect.


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## Body

## 1. Introduction

Hawking radiation is a theoretical argument proposed by Hawking for the existence of thermal radiation emitted by black holes. The standard Hawking formula was first obtained in the frame of quantum field theory in curved spacetime [1]. Afterward, there are various methods for deriving Hawking radiation and calculating its temperature. Among them is a semiclassical method of modeling Hawking radiation as a tunneling effect. This method was first proposed by Kraus and Wilczek [2, 3]. They employed the dynamical geometry approach to calculate the imaginary part of the action for the tunneling process of s-wave emission across the horizon and related it to the Boltzmann factor for the emission at the Hawking temperature. Due to back-reaction effects included, this procedure gives a correction to the standard Hawking temperature formula, which speeds up the process of black holes’ evaporation. An alternative way to calculate the imaginary part of the action is the Hamilton-Jacobi method [4, 5]. Neglecting the self-gravitation, this method assumes that the action of an emitted particle satisfies the relativistic Hamilton-Jacobi equation. Taking the symmetries of the metric into account, one can adopt an appropriate ansatz for the form of the action. Solving the Hamilton-Jacobi equation turns out to recover the standard Hawking temperatures.However, the original Hamilton-Jacobi method proposed in [4, 5] is only confined to the semiclassical approximation and carried out in the framework of the classical general relativity. Beyond the original Hamilton-Jacobi method, there could be some corrections. For simplicity, we use the case of emission of massless scalar with energy E from the Schwarzschild black hole with mass M to illustrate these corrections. In this paper, we set G=c=1, where the Planck constant ħ is of the order of square of the Planck Mass Mp. In these units, the black hole’s horizon rH=2M. The potential corrections to the original Hamilton-Jacobi method are given as follows:(a)
Back-reaction effects, which gives the correction ~E/M: In the Hamilton-Jacobi method, we assume that the metric is fixed and the field is free. Thus, back-reaction effects are disregarded. However, in Parikh and Wilczek method [2, 3], there are back-reaction effects to ensure energy conservation during the emission of a particle via tunneling through the horizon. These corrections lead to nonthermal corrections to the black hole radiation spectrum.(b)
Higher-order WKB corrections: Using WKB approximation method, the lowest order of the equation of motion describing a particle moving in the black hole gives the Hamilton-Jacobi equation. The WKB approximation breaks down when the de Broglie wavelength of the particle,λp~ħ/E, becomes comparable to the horizon of black hole, rH. Therefore, the ratio λp/rH~ħ/EM controls the amount of higher-order WKB corrections. However, several authors [6–8] argued that the tunneling method yields no higher-order corrections to the Hawking temperature.(c)
Corrections from quantum gravity effects: The original Hawking formula predicts the complete evaporation of black holes, which leads to the black hole information paradox (for reviews see [9, 10]). Solving the paradox needs the breakdown of the semiclassical description at the Planck scale. A theory of quantum gravity must be used to describe the final state of black hole evaporation.In this paper, we will investigate the quantum gravity effects on Hawking radiation in the tunneling paradigm. Although a number of quantum gravity theories are proposed, there is still no complete and consistent quantum theory of gravity. Consequently, in the absence of a full quantum description of the black hole evaporation, one uses effective models to describe the quantum gravitational behavior. On the other hand, various theories of quantum gravity, such as string theory, loop quantum gravity, and quantum geometry, predict the existence of a minimal length [11–13]. An effective model to realize this minimal length is the generalized uncertainty principle (GUP). For one-dimensional quantum mechanics, the GUP,(1)Δx^Δp^≥ħ21+βΔp^2,can be obtained from the deformed commutation relation(2)x^,p^=iħ1+βp^2,where β is a small parameter of dimension of inverse momentum squared. In fact, (1) implies an absolute minimum uncertainty of(3)Δxmin=ħβ.The operators can be given in the position representation(4)x^=x,p^=-iħ∂x1-ħ2β∂x2+Oβ2,which is suited best for this paper. When the one-dimensional deformed commutation relation (2) is generalized to D-dimensions, there are several forms available in the literature [14–17]. For example, Kempf et al. [14] modified the multiple-dimensional commutation relations and got(5)xi,pj=iħδij1+βp2,where p2=∑i=1Dpi2 and the generalization preserves the rotational symmetry. Hossenfelder et al. [15] also used modified de Broglie relation approach to get the same commutation relations. When incorporating the GUP into quantum field theory, one needs to generalize D-dimensional deformed commutation relations to include time. However, the existence of the minimal length could lead to Planck scale departures from Lorentz symmetry. Therefore, the corresponding (D+1)-dimensional deformed commutation relations are not Lorentz invariant and give rise to some version of the deformed special relativity. The field theories built on such commutation relations hence do not respect Lorentz symmetry [15, 18–20]. Although Lorentz invariance is not required for the generalization, there are some attempts to introduce (D+1)-dimensional deformed Lorentz invariant generalizations of D-dimensional deformed commutation relations [21, 22]. Thus, the field theories based on these deformed commutation relations are Lorentz invariant. For example, the gauge theories with incorporation of the GUP in [22] are both invariant under Lorentz symmetry and gauge symmetry. In addition, the Klein-Gordon equation described by Quesne-Tkachuk Lorentz-covariant deformed algebra has been given in [23].The standard Hawking formula predicts the complete evaporation of black holes, which leads to the black hole information paradox. There are several approaches to solve the paradox. One of them is that information might be stored in a Planck-sized remnant. This motivates Adler et al. [24] to incorporate the GUP into the derivation of Hawking temperature, which predicts the existence of black hole remnants. The black hole thermodynamics has also been discussed in the GUP framework [25–27]. Incorporating the GUP into the Parikh-Wilczek tunneling mechanism for scalar fields, the corrected Hawking temperatures in the Schwarzschild were obtained [28]. Similarly, one can also use Hamilton-Jacobi method to calculate effects of quantum gravity on particles’ tunneling. Recently, the GUP modified Hamilton-Jacobi equations for fermions in curved spacetime have been introduced and the corrected Hawking temperatures have been derived [29–34].For the Hamilton-Jacobi method, the GUP deformed Klein-Gordon (KG)/Dirac equation in(D+1)-dimensional curved spacetime needs to be first derived. However, different (D+1)-dimensional GUP deformed commutation relations could lead to different deformed KG/Dirac equation. As mentioned previously, there are two kinds of (D+1)-dimensional deformed commutation relations, one of which is Lorentz invariant and the other is not. The field theory built on the Lorentz invariant deformed commutation relations is also Lorentz invariant in flat spacetime. When generalized to curved spacetime using the minimal-coupling principle, the Lorentz invariant deformed Klein-Gordon (KG) equation or Dirac equation becomes covariant. On the other hand, the deformed commutation relations in [15] are not Lorentz invariant and hence the deformed Dirac equation built on them in [30, 31, 33] is not covariant.In this paper, we will study the deformed Hamilton-Jacobi method which incorporates the GUP in a covariant way. In this scenario, we will show that there are no corrections to the Hawking temperature of a black hole from the GUP effects if its original Hawking temperature is independent of the mass of emitted particles. For these purposes, this paper is organized as follows. In Section2, we briefly review the Hamilton-Jacobi method and show that the fermionic Hamilton-Jacobi equation for the action I can be written in the same form of the scalar one. After constructing scalar (fermionic) effective field theories respecting covariance of coordinate spacetime, we derive the deformed model-independent KG/Dirac and Hamilton-Jacobi equations in Section 3. Section 4 is devoted to our discussion and conclusion.


## 2. Hamilton-Jacobi Method

In this section, we briefly review how to calculate the imaginary part of the action making use of the Hamilton-Jacobi equation [4]. This semiclassical method models Hawking radiation as tunneling through the horizon. Using the WKB approximation the tunneling probability for the classically forbidden trajectory through the horizon is given by(6)Γ∝exp⁡-2ImIħ,where I is the classical action of the trajectory. One can relate Γ to the Boltzmann factor for the emission from the black hole to get Hawking temperature.


### 2.1. Scalar Field

The equation satisfied by the scalar field is(7)DμDμϕ+m2ħ2ϕ=∇μ+ieħAμ∇μ+ieħAμϕ+m2ħ2ϕ=0,where ∇μ is the covariant derivative of the black hole and Aμ is its electromagnetic potential. Making the ansatz for ϕ, which is(8)ϕ=exp⁡iIħ,and substituting it into (7), one expands (7) in powers of ħ and finds the lowest order(9)∂μI+eAμ∂μI+eAμ-m2=0.Equation (9) is just the Hamilton-Jacobi equation satisfied by a scalar particle of mass m moving in the black hole with the electromagnetic potential Aμ. The solution to (9) is the action of the scalar’s classically forbidden trajectory through the horizon.To illustrate how the Hamilton-Jacobi method works, we consider Hawking radiation in the1+1-dimensional Schwarzschild black hole with line element (with c=G=1)(10)ds2=1-2Mrdt2-1-2Mr-1dr2.Thus, (9) becomes(11)1-2Mr-1∂tI2-1-2Mr∂rI2-m2=0,where we use Aμ=0 for the Schwarzschild black hole. Using the method of separation of variables, we find that the solution to the above equation is(12)I±=-Et∓∫dr1-2M/rE2-m21-2Mr,where E is a constant and +- corresponds to the outgoing (ingoing) solutions. Choosing the contour to lie in the upper complex plane, one gets that the imaginary part of I is (13)ImI±=∓∫2M-ϵ2M+ϵdr1-2M/rE2-m21-2Mr=±2πEM.Thus, the tunneling rate is(14)Γ=PemissionPabsorption=exp⁡-2ImI+exp⁡-2ImI-=exp⁡-8πME.Comparing the above equation with the Boltzmann factor at the Hawking temperature near the event horizon gives(15)T=18πM.


### 2.2. Fermion Field

In curved spacetime, the Dirac equation for a spin-1/2 fermion with an electromagnetic field Aμ takes on the form(16)iγμ∂μ+Ωμ+ieħAμψ-mħψ=0,where Ωμ≡i/2ωμabΣab, Σab is the Lorentz spinor generator, ωμab is the spin connection, and γμ,γν=2gμν. The Greek indices are raised and lowered by the curved metric gμν, while the Latin indices are governed by the flat metric ηab. To obtain the Hamilton-Jacobi equation for a fermion, the ansatz for ψ is assumed as (17)ψ=exp⁡iIħv,where v is a slowly varying spinor amplitude. Substituting (17) into (16), we find to the lowest order of ħ(18)γμ∂μI+eAμv=-mv,which is the Hamilton-Jacobi equation satisfied by a fermion particle of mass m moving in the black hole with the electromagnetic potential Aμ. Solving (18) gives us the classical action I. Multiplying both sides of (18) from the left by γν∂νI+eAv and then using (18) to simplify the RHS, one gets(19)γν∂νI+eAvγμ∂μI+eAμv=m2v.Manipulating the LHS of the above equation by using γμ,γν=2gμν, we have(20)∂μI+eAμ∂μI+eAμ-m2v=0.Since v is nonzero, the Hamilton-Jacobi equation satisfied by the classical action I for a fermion finally becomes(21)∂μI+eAμ∂μI+eAμ-m2=0,which is the same as the Hamilton-Jacobi equation for a scalar with the same mass m, namely, (9).


## 2.1. Scalar Field

The equation satisfied by the scalar field is(7)DμDμϕ+m2ħ2ϕ=∇μ+ieħAμ∇μ+ieħAμϕ+m2ħ2ϕ=0,where ∇μ is the covariant derivative of the black hole and Aμ is its electromagnetic potential. Making the ansatz for ϕ, which is(8)ϕ=exp⁡iIħ,and substituting it into (7), one expands (7) in powers of ħ and finds the lowest order(9)∂μI+eAμ∂μI+eAμ-m2=0.Equation (9) is just the Hamilton-Jacobi equation satisfied by a scalar particle of mass m moving in the black hole with the electromagnetic potential Aμ. The solution to (9) is the action of the scalar’s classically forbidden trajectory through the horizon.To illustrate how the Hamilton-Jacobi method works, we consider Hawking radiation in the1+1-dimensional Schwarzschild black hole with line element (with c=G=1)(10)ds2=1-2Mrdt2-1-2Mr-1dr2.Thus, (9) becomes(11)1-2Mr-1∂tI2-1-2Mr∂rI2-m2=0,where we use Aμ=0 for the Schwarzschild black hole. Using the method of separation of variables, we find that the solution to the above equation is(12)I±=-Et∓∫dr1-2M/rE2-m21-2Mr,where E is a constant and +- corresponds to the outgoing (ingoing) solutions. Choosing the contour to lie in the upper complex plane, one gets that the imaginary part of I is (13)ImI±=∓∫2M-ϵ2M+ϵdr1-2M/rE2-m21-2Mr=±2πEM.Thus, the tunneling rate is(14)Γ=PemissionPabsorption=exp⁡-2ImI+exp⁡-2ImI-=exp⁡-8πME.Comparing the above equation with the Boltzmann factor at the Hawking temperature near the event horizon gives(15)T=18πM.


## 2.2. Fermion Field

In curved spacetime, the Dirac equation for a spin-1/2 fermion with an electromagnetic field Aμ takes on the form(16)iγμ∂μ+Ωμ+ieħAμψ-mħψ=0,where Ωμ≡i/2ωμabΣab, Σab is the Lorentz spinor generator, ωμab is the spin connection, and γμ,γν=2gμν. The Greek indices are raised and lowered by the curved metric gμν, while the Latin indices are governed by the flat metric ηab. To obtain the Hamilton-Jacobi equation for a fermion, the ansatz for ψ is assumed as (17)ψ=exp⁡iIħv,where v is a slowly varying spinor amplitude. Substituting (17) into (16), we find to the lowest order of ħ(18)γμ∂μI+eAμv=-mv,which is the Hamilton-Jacobi equation satisfied by a fermion particle of mass m moving in the black hole with the electromagnetic potential Aμ. Solving (18) gives us the classical action I. Multiplying both sides of (18) from the left by γν∂νI+eAv and then using (18) to simplify the RHS, one gets(19)γν∂νI+eAvγμ∂μI+eAμv=m2v.Manipulating the LHS of the above equation by using γμ,γν=2gμν, we have(20)∂μI+eAμ∂μI+eAμ-m2v=0.Since v is nonzero, the Hamilton-Jacobi equation satisfied by the classical action I for a fermion finally becomes(21)∂μI+eAμ∂μI+eAμ-m2=0,which is the same as the Hamilton-Jacobi equation for a scalar with the same mass m, namely, (9).


## 3. Hamilton-Jacobi Equation Incorporating GUP

To incorporate the GUP into the Hamilton-Jacobi method, we need to derive the KG/Dirac equations in the framework of the GUP. As mentioned in the Introduction, there are a lot of attempts to introduce the GUP into quantum field theory. If the field theory is built on the Lorentz invariant deformed commutation relations, the deformed KG/Dirac equations are covariant in curved spacetime. In this section, we will calculate the Hawking radiation in the framework of the covariant deformed KG/Dirac equations by making use of the Hamilton-Jacobi method.


### 3.1. Model-Independent Covariant Deformed KG/Dirac Equations

The forms of the covariant deformed KG/Dirac equations depend on the deformed commutation relations which we use. To be as general as possible, in this paper we will not resort to any specific model. Instead, we will derive the model-independent covariant deformed KG/Dirac equations by considering effective field theories respecting covariance. For the charged black hole background, theU1 gauge invariance of the effective field theory is assumed as well. We also assume introducing the GUP to the original field theory does not make a stable particle unstable. Now that the original field theory is free, there are no self-interacting effective operators in the effective field theories. Thus, the effective Lagrangian involving the scalar field ϕ (fermion field ψ) in the background of a D+1-dimensional black hole with the electromagnetic potential Aμ is given by(22)Leffsf=∑n,jCn,jsfΛn-D+1On,jsf,where sf denotes the scalar (fermion), the n≥D+1 denotes the operator dimension, j runs over all independent operators of a given dimension, and Λ is the energy scale related to the minimal length lmin, Λ~ħ/lmin. The lowest dimensional operator with n=D+1 is the original free field Lagrangian in curved spacetime with the electromagnetic potential Aμ: (23)OD+1s=-ϕ+DμDμ+m2ħ2ϕ,OD+1f=ψ-iDμfγμ-mħψ,where Dμ≡∇μ+ie/ħAμ,Dμf≡∂μ+Ωμ+ie/ħAμ, and m is the mass of the particle. For the fermion field ψ, the basis of independent effective operators with n=D+2 is given by(24)OD+2,1f=ħψ-γνDνfγμDμfψ,OD+2,2f=ħψ-Df,μDμfψ,OD+2,3f=imψ-γμDμfψ,OD+2,4f=m2ħψ-ψ.For the scalar field ϕ, the operator with n=D+2 which are gauge-invariant and covariant is (25)OD+2s=mϕ+DμDμϕ.If we truncate the scalar effective theory at O1/Λ, by redefining the scalar field ϕ, it is easy to see that the truncated effective theory is equivalent to the original field theory with redefined mass. So we need effective operators at O1/Λ2 to produce nontrivial results. The basis of independent effective operators with n=D+3 is(26)OD+3,1s=ħ2ϕ+DμDμDνDνϕ,OD+3,2s=ħ2ϕ+DμDνDνDμϕ,OD+3,3s=ħ2ϕ+DμDνDμDνϕ,OD+3,4s=m2ϕ+DμDμϕ,OD+3,5s=m4ħ2ϕ+ϕ.Define the action Seffsf=∫dD+1xgLeffsf. Varying Seffsf with respect to ϕ+ψ- gives the deformed KG (Dirac) equation of ϕψ. Thus, the deformed KG equation to O1/Λ2 is (27)-DμDμϕ-m2ħ2ϕ+CD+2smΛDμDμϕ+CD+3,1sħ2Λ2DμDμDνDνϕ+CD+3,2sħ2Λ2DμDνDνDμϕ+CD+3,3sħ2Λ2DμDνDμDνϕ+CD+3,4sm2Λ2DμDμϕ+CD+3,5sΛ2m4ħ2ϕ=0,and the deformed Dirac equation to O1/Λ is(28)iγμDμfψ-mħψ+CD+2,1fħΛγνDνfγμDμfψ+CD+2,2fħΛDf,μDμfψ+iCD+2,3fmΛγμDμfψ+CD+2,4fΛm2ħψ=0.


### 3.2. Deformed Scalar Hamilton-Jacobi Equation

To find the classical actionI by using WKB approximation to solve (27), we make the ansatz for ϕ as before (29)ϕ=exp⁡iIħ.Substituting it into (27), one expands (27) in powers of ħ and finds the lowest order(30)A∂μI+eAμ∂μI+eAμ-Bm2+CΛ2∂μI+eAμ∂μI+eAμ2=0,where A=1-CD+2sm/Λ-CD+3,4sm2/Λ2,B=1+CD+3,5sm2/Λ2, and C≡CD+3,1s+CD+3,2s+CD+3,3s. Solving (30) gives(31)∂μI+eAμ∂μI+eAμ=meff,±2,where(32)meff,±2≡-A±A2+4BCm2Λ-22CΛ2.When m/Λ→0, we find meff,+2~m2 and meff,-2~-2/CΛ2. As Λ≫m, (31) gives ∂μI~Λ for meff,-2 and hence the action I highly oscillates in spacetime. One may argue such action is not physical and hence could be discarded by using the low-momentum consistency condition proposed in [35]. Alternatively, one wants to recover the results without the GUP when Λ→∞. However, as Λ→∞, the solution to (31) with meff,-2 blows up while (31) with meff,+2 becomes (9) since meff,+2→m2. Therefore, we pick meff,+2 in (31). Comparing (31) with (9), we find that all the GUP contributions to the deformed scalar Hamilton-Jacobi equation are included in one effective parameter, meff2.


### 3.3. Deformed Fermionic Hamilton-Jacobi Equation

To obtain the Hamilton-Jacobi equation for the classical action, the ansatz forψ takes the form of (33)ψ=exp⁡iIħv,where v is a vector function of the spacetime. Substituting (33) into (28), we find the lowest order of ħ(34)-Aγμ∂μI+eAμv=Bm+CΛ∂μI+eAμ∂μI+eAμv,where A=1+CD+2,3fm/Λ,B=1+CD+2,4fm/Λ, and C≡CD+2,1f+CD+2,2f. Multiplying both sides of (34) from the left by -Aγν∂νI+eAv and using (34) on RHS, we obtain(35)A2∂μI+eAμ∂μI+eAμ=Bm+CΛ∂μI+eAμ∂μI+eAμ2.Solving (35), we also find(36)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is a function of m, Λ, A, B, and C and is chosen as meff2→m2 as Λ→∞. Similarly, all the GUP contributions to the deformed fermionic Hamilton-Jacobi equation are included in one effective parameter, meff2.


### 3.4. Deformed Hamilton-Jacobi Equation to All Orders

We have shown that the deformed scalar (fermionic) Hamilton-Jacobi equation can be written as the form of (36) up to the order of 1/Λ21/Λ. Here, we will show that the deformed scalar (fermionic) Hamilton-Jacobi equation can also be written as the form of (36) to all orders of the effective theories.For a scalar field, the effective operatorOn,js must contain even number of Dμ to be covariant. Since On,js contains two ϕ, we find (37)On,js=ħ2q-2mpϕ+CDμ1⋯Dμ2qϕ,where integers p,q⩾0,2q+p=n-D+1,j=C,p and C denotes any possible way of contracting μ1⋯μ2q in pair to make On,js covariant. Therefore, the deformed KG equation to all orders of the effective theory is(38)-DμDμϕ-m2ħ2ϕ+∑j,n>D+1Cn,jsħ2q-2mpΛn-D+1CDμ1⋯Dμ2qϕ=0.Making the ansatz ϕ=exp⁡iI/ħ and substituting it into (36) gives the deformed Hamilton-Jacobi equation for I:(39)GX≡X-m2+fX=0,where X≡∂μI+eAμ∂μI+eAμ and (40)fx≡∑j,n>D+1-1qCn,jsmpxqΛn-D+1.When m/Λ≪1 as assumed, for (39), there exists one and only one root meff2 in 0,2m2. In fact, since m/Λ≪1, f0 and f2m2~m2m/Λ≪m2. Thus, one finds G0<0 and G2m2>0. So there exists one root of (39) in 0,2m2. On the other hand, using f′x~m/Λ≪1 for x∈0,2m2, one finds G′x>0 for x∈0,2m2. This completes the proof of existence of one and only one root of (39) in 0,2m2. There might be other roots which are not in 0,2m2. However, they are not physical and discarded since they do not approach m2 as Λ→∞. By solving (39), we find that the classical action I satisfies (41)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is uniquely determined by Λ, m, and Cn,js.For a fermion field, the effective operatorOn,jf can be written as(42)On,jf=iqħq-1mpψ-CDμ1f⋯Dμqfγν1⋯γν2r-qψ,where integers q,p,r⩾0,p+q=n-D,q⩾r⩾q/2,j=C,q,r and C denotes any possible way of contracting μ1⋯μq and ν1⋯ν2r-q in pair. Therefore, the deformed Dirac equation to all orders of the effective theory is(43)iγμDμfψ-mħψ+∑j,n>D+1Cn,jfiqħq-1mpΛn-D+1CDμ1f⋯Dμqfγν1⋯γν2r-qψ=0.Substituting the ansatz ψ=expiI/ħv into (43), we find to the lowest order of ħ:(44)1-gXγμ∂μI+eAμv=fX-mv,where X≡∂μI+eAμ∂μI+eAμ and(45)fx≡∑j,n>D+1,qis  evenCn,jfmpxq/2Λn-D+1,gx≡∑j,n>D+1,qis  odd-Cn,jfmpxq-1/2Λn-D+1.Using the same manipulation as before, we find that (44) reduces to(46)HX≡1-gX2X-fX-m2=0.For m/Λ≪1, one can show that f0, f2m2≪m and g0, g2m2≪1. Thus, H0<0 and H2m2>0. Moreover, H′x>0 for x∈0,2m2 since f′x≪1 and xg′x≪1 for x∈0,2m2. Therefore, there exists one and only one root meff2 of (46) in 0,2m2. (46) leads to (47)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is uniquely determined by Λ, m, and Cn,jf.


## 3.1. Model-Independent Covariant Deformed KG/Dirac Equations

The forms of the covariant deformed KG/Dirac equations depend on the deformed commutation relations which we use. To be as general as possible, in this paper we will not resort to any specific model. Instead, we will derive the model-independent covariant deformed KG/Dirac equations by considering effective field theories respecting covariance. For the charged black hole background, theU1 gauge invariance of the effective field theory is assumed as well. We also assume introducing the GUP to the original field theory does not make a stable particle unstable. Now that the original field theory is free, there are no self-interacting effective operators in the effective field theories. Thus, the effective Lagrangian involving the scalar field ϕ (fermion field ψ) in the background of a D+1-dimensional black hole with the electromagnetic potential Aμ is given by(22)Leffsf=∑n,jCn,jsfΛn-D+1On,jsf,where sf denotes the scalar (fermion), the n≥D+1 denotes the operator dimension, j runs over all independent operators of a given dimension, and Λ is the energy scale related to the minimal length lmin, Λ~ħ/lmin. The lowest dimensional operator with n=D+1 is the original free field Lagrangian in curved spacetime with the electromagnetic potential Aμ: (23)OD+1s=-ϕ+DμDμ+m2ħ2ϕ,OD+1f=ψ-iDμfγμ-mħψ,where Dμ≡∇μ+ie/ħAμ,Dμf≡∂μ+Ωμ+ie/ħAμ, and m is the mass of the particle. For the fermion field ψ, the basis of independent effective operators with n=D+2 is given by(24)OD+2,1f=ħψ-γνDνfγμDμfψ,OD+2,2f=ħψ-Df,μDμfψ,OD+2,3f=imψ-γμDμfψ,OD+2,4f=m2ħψ-ψ.For the scalar field ϕ, the operator with n=D+2 which are gauge-invariant and covariant is (25)OD+2s=mϕ+DμDμϕ.If we truncate the scalar effective theory at O1/Λ, by redefining the scalar field ϕ, it is easy to see that the truncated effective theory is equivalent to the original field theory with redefined mass. So we need effective operators at O1/Λ2 to produce nontrivial results. The basis of independent effective operators with n=D+3 is(26)OD+3,1s=ħ2ϕ+DμDμDνDνϕ,OD+3,2s=ħ2ϕ+DμDνDνDμϕ,OD+3,3s=ħ2ϕ+DμDνDμDνϕ,OD+3,4s=m2ϕ+DμDμϕ,OD+3,5s=m4ħ2ϕ+ϕ.Define the action Seffsf=∫dD+1xgLeffsf. Varying Seffsf with respect to ϕ+ψ- gives the deformed KG (Dirac) equation of ϕψ. Thus, the deformed KG equation to O1/Λ2 is (27)-DμDμϕ-m2ħ2ϕ+CD+2smΛDμDμϕ+CD+3,1sħ2Λ2DμDμDνDνϕ+CD+3,2sħ2Λ2DμDνDνDμϕ+CD+3,3sħ2Λ2DμDνDμDνϕ+CD+3,4sm2Λ2DμDμϕ+CD+3,5sΛ2m4ħ2ϕ=0,and the deformed Dirac equation to O1/Λ is(28)iγμDμfψ-mħψ+CD+2,1fħΛγνDνfγμDμfψ+CD+2,2fħΛDf,μDμfψ+iCD+2,3fmΛγμDμfψ+CD+2,4fΛm2ħψ=0.


## 3.2. Deformed Scalar Hamilton-Jacobi Equation

To find the classical actionI by using WKB approximation to solve (27), we make the ansatz for ϕ as before (29)ϕ=exp⁡iIħ.Substituting it into (27), one expands (27) in powers of ħ and finds the lowest order(30)A∂μI+eAμ∂μI+eAμ-Bm2+CΛ2∂μI+eAμ∂μI+eAμ2=0,where A=1-CD+2sm/Λ-CD+3,4sm2/Λ2,B=1+CD+3,5sm2/Λ2, and C≡CD+3,1s+CD+3,2s+CD+3,3s. Solving (30) gives(31)∂μI+eAμ∂μI+eAμ=meff,±2,where(32)meff,±2≡-A±A2+4BCm2Λ-22CΛ2.When m/Λ→0, we find meff,+2~m2 and meff,-2~-2/CΛ2. As Λ≫m, (31) gives ∂μI~Λ for meff,-2 and hence the action I highly oscillates in spacetime. One may argue such action is not physical and hence could be discarded by using the low-momentum consistency condition proposed in [35]. Alternatively, one wants to recover the results without the GUP when Λ→∞. However, as Λ→∞, the solution to (31) with meff,-2 blows up while (31) with meff,+2 becomes (9) since meff,+2→m2. Therefore, we pick meff,+2 in (31). Comparing (31) with (9), we find that all the GUP contributions to the deformed scalar Hamilton-Jacobi equation are included in one effective parameter, meff2.


## 3.3. Deformed Fermionic Hamilton-Jacobi Equation

To obtain the Hamilton-Jacobi equation for the classical action, the ansatz forψ takes the form of (33)ψ=exp⁡iIħv,where v is a vector function of the spacetime. Substituting (33) into (28), we find the lowest order of ħ(34)-Aγμ∂μI+eAμv=Bm+CΛ∂μI+eAμ∂μI+eAμv,where A=1+CD+2,3fm/Λ,B=1+CD+2,4fm/Λ, and C≡CD+2,1f+CD+2,2f. Multiplying both sides of (34) from the left by -Aγν∂νI+eAv and using (34) on RHS, we obtain(35)A2∂μI+eAμ∂μI+eAμ=Bm+CΛ∂μI+eAμ∂μI+eAμ2.Solving (35), we also find(36)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is a function of m, Λ, A, B, and C and is chosen as meff2→m2 as Λ→∞. Similarly, all the GUP contributions to the deformed fermionic Hamilton-Jacobi equation are included in one effective parameter, meff2.


## 3.4. Deformed Hamilton-Jacobi Equation to All Orders

We have shown that the deformed scalar (fermionic) Hamilton-Jacobi equation can be written as the form of (36) up to the order of 1/Λ21/Λ. Here, we will show that the deformed scalar (fermionic) Hamilton-Jacobi equation can also be written as the form of (36) to all orders of the effective theories.For a scalar field, the effective operatorOn,js must contain even number of Dμ to be covariant. Since On,js contains two ϕ, we find (37)On,js=ħ2q-2mpϕ+CDμ1⋯Dμ2qϕ,where integers p,q⩾0,2q+p=n-D+1,j=C,p and C denotes any possible way of contracting μ1⋯μ2q in pair to make On,js covariant. Therefore, the deformed KG equation to all orders of the effective theory is(38)-DμDμϕ-m2ħ2ϕ+∑j,n>D+1Cn,jsħ2q-2mpΛn-D+1CDμ1⋯Dμ2qϕ=0.Making the ansatz ϕ=exp⁡iI/ħ and substituting it into (36) gives the deformed Hamilton-Jacobi equation for I:(39)GX≡X-m2+fX=0,where X≡∂μI+eAμ∂μI+eAμ and (40)fx≡∑j,n>D+1-1qCn,jsmpxqΛn-D+1.When m/Λ≪1 as assumed, for (39), there exists one and only one root meff2 in 0,2m2. In fact, since m/Λ≪1, f0 and f2m2~m2m/Λ≪m2. Thus, one finds G0<0 and G2m2>0. So there exists one root of (39) in 0,2m2. On the other hand, using f′x~m/Λ≪1 for x∈0,2m2, one finds G′x>0 for x∈0,2m2. This completes the proof of existence of one and only one root of (39) in 0,2m2. There might be other roots which are not in 0,2m2. However, they are not physical and discarded since they do not approach m2 as Λ→∞. By solving (39), we find that the classical action I satisfies (41)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is uniquely determined by Λ, m, and Cn,js.For a fermion field, the effective operatorOn,jf can be written as(42)On,jf=iqħq-1mpψ-CDμ1f⋯Dμqfγν1⋯γν2r-qψ,where integers q,p,r⩾0,p+q=n-D,q⩾r⩾q/2,j=C,q,r and C denotes any possible way of contracting μ1⋯μq and ν1⋯ν2r-q in pair. Therefore, the deformed Dirac equation to all orders of the effective theory is(43)iγμDμfψ-mħψ+∑j,n>D+1Cn,jfiqħq-1mpΛn-D+1CDμ1f⋯Dμqfγν1⋯γν2r-qψ=0.Substituting the ansatz ψ=expiI/ħv into (43), we find to the lowest order of ħ:(44)1-gXγμ∂μI+eAμv=fX-mv,where X≡∂μI+eAμ∂μI+eAμ and(45)fx≡∑j,n>D+1,qis  evenCn,jfmpxq/2Λn-D+1,gx≡∑j,n>D+1,qis  odd-Cn,jfmpxq-1/2Λn-D+1.Using the same manipulation as before, we find that (44) reduces to(46)HX≡1-gX2X-fX-m2=0.For m/Λ≪1, one can show that f0, f2m2≪m and g0, g2m2≪1. Thus, H0<0 and H2m2>0. Moreover, H′x>0 for x∈0,2m2 since f′x≪1 and xg′x≪1 for x∈0,2m2. Therefore, there exists one and only one root meff2 of (46) in 0,2m2. (46) leads to (47)∂μI+eAμ∂μI+eAμ=meff2,where meff2 is uniquely determined by Λ, m, and Cn,jf.


## 4. Discussion and Conclusion

The Hamilton-Jacobi method without and with the incorporation of the GUP has been studied in this paper. Specifically, we have calculated the scalar and fermionic Hamilton-Jacobi equations for the classical actionI in the background of a D+1-dimensional black hole with the metric gμν and the electromagnetic potential Aμ. First, in Section 2, we revisited the derivation of the usual Hamilton-Jacobi equations for the action I of tunneling of scalar and fermionic particles from the black hole. In the framework of effective field theories expanded in powers of 1/Λ constructed in Section 3, the deformed model-independent KG/Dirac equations respecting covariance and gauge invariance of Aμ have then been derived. Finally, substituting the WKB ansatz for the scalar and fermionic wavefunctions into the deformed KG/Dirac equations, we expanded them in powers of ħ, kept only the lowest order, and hence gave the deformed Hamilton-Jacobi equations. The deformed scalar (fermionic) Hamilton-Jacobi equations to O1/Λ2O1/Λ are derived in Section 3 while the deformed Hamilton-Jacobi equations to all orders of the effective field theories are also given there.Our results are summarized as follows:(a)
In the case of no GUP, we have shown in Section2 that the fermionic Hamilton-Jacobi equation for the action I can be written in the same form of the scalar one. Both can be written as (48)∂μI+eAμ∂μI+eAμ=m2,whereAμ is the black hole’s electromagnetic potential and m is the mass of the particle.(b)
In the case of incorporating the GUP into quantum field theory in a covariant way, we have shown in Section3 that both scalar and fermionic deformed Hamilton-Jacobi equations can be reduced to (49)∂μI+eAμ∂μI+eAμ=meff2,where all the GUP contributions are included in only one parametermeff2.As a bonus of result (a), it provides a shortcut to calculate the actionI of tunneling of a fermionic particle from the black hole. Instead of solving the complicated matrix equation (18), we can solve (48) for I. For example, such shortcut was discussed in the case of fermion tunneling from the Bardeen-Vaidya black hole in [36]. Since both scalar and fermion actions satisfy the same equation (48), the Hamilton-Jacobi method relating the imaginary part of the actions to Hawking temperature indicates that Hawking temperatures for scalar and fermion particles are the same. In fact, using the Hamilton-Jacobi method, Hawking temperatures were calculated for a scalar and a fermion, in the context of charged BTZ black holes [37], black strings [38, 39], and so forth, and same results were found. As shown above, the coincidence is guaranteed by (48).For the standard Hawing radiation, all particles very close to the horizon are effectively massless on account of infinite blueshift. Thus, the conformal invariance of the horizon makes Hawing temperatures of all particles the same. The mass, angular momentum, and identity of the particles are only relevant when they escape the potential barrier. This is what our result (a) gives. However, if quantum gravity effects are considered, behaviors of particles near the horizon could be different. For example, if we send a wave packet which is governed by a subluminal dispersion relation, backwards in time toward the horizon, it reaches a minimum distance of approach, then reverses direction, and propagates back away from the horizon, instead of getting unlimited blueshift toward the horizon [40, 41]. Thus, quantum gravity effects might make fermions and scalars experience different (effective) Hawking temperatures. However, our result shows that in the covariant GUP models, the Hawing temperatures of scalars and fermions are the same, independently of their angular momentums and identities.When incorporating the GUP into quantum field theory, as mentioned in the Introduction, there are two kinds of realizations, one of which respects covariance and the other does not. For the noncovariant realization, the deformed Hamilton-Jacobi method incorporated with the GUP was studied in [29–34]. There, it has been shown that the corrections to the standard Hawking temperature depend on the masses and angular momentums of the emitted particles in a nontrivial way. In some cases, such corrections could lead to the remnant being left in the evaporation [29–31].In this paper, we investigated the deformed Hamilton-Jacobi method for a GUP modified QFT, which incorporates the GUP in a covariant way. For this Lorentz invariant GUP modified QFT, we found that the effect of GUP on the Hamilton-Jacobi equations was simply to “renormalize” the mass of the emitted particles, fromm to meff. Note that the original Hawking temperature is independent of the mass of emitted particles. As a consequence, there is no correction from the GUP to the Hawking temperature for a Lorentz invariant GUP modified QFT. Therefore, one may argue that covariance of incorporating the GUP into quantum field theory has to be broken in order to have the remnant left in the evaporation.



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*Source: 3191839-2017-12-18.xml*