Black hole evaporation in Hořava–Lifshitz gravity

Abstract

Hořava–Lifshitz (HL) gravity was formulated in hope of solving the non-renormalization problem in Einstein gravity and the ghost problem in higher derivative gravity theories by violating Lorentz invariance. In this work we consider the spherically symmetric neutral AdS black hole evaporation process in HL gravity in various spacetime dimensions d, and with detailed balance violation parameter $$0\leqslant \epsilon ^2\leqslant 1$$ 0 ⩽ ϵ 2 ⩽ 1 . We find that the lifetime of the black holes under Hawking evaporation is dimensional dependent, with $$d=4,5$$ d = 4 , 5 behave differently from $$d\geqslant 6$$ d ⩾ 6 . For the case of $$\epsilon =0$$ ϵ = 0 , in $$d=4,5$$ d = 4 , 5 , the black hole admits zero temperature state, and the lifetime of the black hole is always infinite. This phenomenon obeys the third law of black hole thermodynamics, and implies that the black holes become an effective remnant towards the end of the evaporation. As $$d\geqslant 6$$ d ⩾ 6 , however, the lifetime of black hole does not diverge with any initial black hole mass, and it is bounded by a time of the order of $$\ell ^{d-1}$$ ℓ d - 1 , similar to the case of Schwarzschild-AdS in Einstein gravity (which corresponds to $$\epsilon ^2=1$$ ϵ 2 = 1 ), though for the latter this holds for all $$d\geqslant 4$$ d ⩾ 4 . The case of $$0<\epsilon ^2<1$$ 0 < ϵ 2 < 1 is also qualitatively similar with $$\epsilon =0$$ ϵ = 0 .

Hawking evaporation of Einstein–Gauss–Bonnet AdS black holes in $$D\geqslant 4$$ dimensions

“…Also, in the cases D = 4, 5 there always have remnants, while in the cases D 6 that all the black holes will evaporate in a finite time. This phenomenon is quite similar to the Hořava-Lifshitz case [23], which also has the dimensional dependent evaporation behavior.…”

“…If we obtain the impact factor b c , we can get the Hawking emission rate in D-dimensional spacetime according to Stefan-Boltzmann law, yields [10,21,23,64,65]…”

“…This is because although the black hole may have infinite initial mass, the temperature, and also the particles' emission power, are also divergent, thus the infinite amount of mass can be evaporated away in a finite time. The study on black holes evaporation in asymptotically AdS spacetimes have been extended to many different backgrounds, such as Lovelock gravity [21], Conformal (Weyl) Gravity [22], Hořava-Lifshitz gravity [23], and dRGT massive gravity [24], etc.…”

Model parameters in the context of late time cosmic acceleration in $f(Q,T)$ gravity

“…The motivation behind such a geometrically extended gravity is to address the late time cosmic phenomena issue. Xu et al [22] also suggested the Weyl type f (Q, T ) gravity and its cosmological implications. Zia et al [23] have obtained the cosmological model in f (Q, T ) gravity applying the energy conservation equation.…”

Constraining effective equation of state in f(Q, T) gravity

“…After that, Yixin et al [33,34] introduced a symmetric teleparallel gravity extension based on the coupling between non-metricity Q and the trace of the energy-momentum tensor T , i.e., considering an arbitrary function f (Q, T ) in the gravitational action. Using some functional forms of f (Q, T ), some works in this modified gravity look at cosmological models and rapid expansion of the universe.…”