Hawking evaporation of black holes in massive gravity

Hou, Meng-Shi; Xu, Hao; Ong, Yen Chin

doi:10.1140/epjc/s10052-020-08678-1

Cited by 23 publications

(18 citation statements)

References 42 publications

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“…For the massless case, the crucial contribution to the greybody factor directly depends on the distance between two horizons as shown in Eq. (45). As a result, the greybody factor which is equivalent to the transmission coefficient significantly depends on the shape of the potential.…”

Section: Discussionmentioning

confidence: 99%

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Greybody factor for black holes in dRGT massive gravity

Boonserm¹,

Ngampitipan²,

Wongjun³

2018

Eur. Phys. J. C

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In general relativity, greybody factor is a quantity related to the quantum nature of a black hole. A high value of greybody factor indicates a high probability that Hawking radiation can reach infinity. Although general relativity is correct and has been successful in describing many phenomena, there are some questions that general relativity cannot answer. Therefore, general relativity is often modified to attain answers. One of the modifications is the 'massive gravity'. The viable model of the massive gravity theory belongs to de Rham, Gabadadze and Tolley (dRGT). In this paper, we calculate the gravitational potential for the de Sitter black hole and for the dRGT black hole. We also derive the rigorous bound on the greybody factor for the de Sitter black hole and the dRGT black hole. It is found that the structure of potentials determines how much the rigorous bound on the greybody factor should be. That is, the higher the potential, the lesser the bound on the greybody factor will be. Moreover, we compare the greybody factor derived from the rigorous bound with the greybody factor derived from the matching technique. The result shows that the rigorous bound is a true lower bound because it is less than the greybody factor obtained from the matching technique.

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Section: Discussionmentioning

confidence: 99%

“…In the context of Hawking radiation, there are various kinds of fluctuation fields treated as the radiation while the massless case in dRGT massive gravity has been investigated recently [45]. Therefore, studies of greybody factors around the black hole depends on particular fields.…”

Section: Introductionmentioning

confidence: 99%

Greybody factor for black holes in dRGT massive gravity

Boonserm¹,

Ngampitipan²,

Wongjun³

2018

Eur. Phys. J. C

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“…These restrictions are summarized in Table 1. It should be remarked that there is no ambiguity on which sign should be considered in front of the square root in the expression for R r once the range of the parameters is decided, and that remnants in massive gravity can exist in both asymptotically de Sitter and anti-de Sitter spacetimes (the analysis in [88,89] only assumed one possibility for the sign in (48)).…”

Section: R Rmentioning

confidence: 99%

A critical assessment of black hole solutions with a linear term in their redshift function

2021

Self Cite

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Different theories of gravity can admit the same black hole solution, but the parameters usually have different physical interpretations. In this work we study in depth the linear term $$\beta r$$ β r in the redshift function of black holes, which arises in conformal gravity, de Rham–Gabadadze–Tolley (dRGT) massive gravity, f(R) gravity (as approximate solution) and general relativity. Geometrically we quantify the parameter $$\beta $$ β in terms of the curvature invariants. Astrophysically we found that $$\beta $$ β can be expressed in terms of the cosmological constant, the photon orbit radius and the innermost stable circular orbit (ISCO) radius. The metric degeneracy can be broken once black hole thermodynamics is taken into account. Notably, we show that under Hawking evaporation, different physical theories with the same black hole solution (at the level of the metric) can lead to black hole remnants with different values of their physical masses with direct consequences on their viability as dark matter candidates. In particular, the mass of the graviton in massive gravity can be expressed in terms of the cosmological constant and of the formation epoch of the remnant. Furthermore the upper bound of remnant mass can be estimated to be around $$0.5 \times 10^{27}$$ 0.5 × 10 27 kg.

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“…The most important achievements in the astrophysics context are: the existence of white dwarfs more than the Chandrasekhar limit [80], and massive neutron stars with maximum mass more than three times the solar mass [81]. To name a few in the point of black hole physics, one can mention: the existence of van der Waals like behavior in extended phase space for non-spherical black holes [82,83], triple points and N-fold reentrant phase transitions [84], the existence of a remnant for a black hole which may help to ameliorate the information paradox [85,86], etc.…”

Section: Introductionmentioning

confidence: 99%

Three-dimensional AdS black holes in massive-power-Maxwell theory

Panah¹,

Jafarzade²,

Rincon³

2022

Preprint

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Recently, it was shown that power-Maxwell (PM) theory can remove the singularity of electric field [1]. Motivated by great interest in three-dimensional black holes and a surge of success in studying massive gravity from both the cosmological and astrophysical point of view, we investigate such black hole solutions in de Rham, Gabadadze and Tolley (dRGT) massive theory of gravity in the presence of PM electrodynamics. First, we extract exact three-dimensional solutions in the PM-dRGT massive gravity. Then we study geometrical properties including type of singularity and asymptotic behavior, and show that although there is a singularity at the origin for asymptotical (A)dS, only AdS solutions are covered by an event horizon. Calculating conserved and thermodynamic quantities, we check the validity of the first law of thermodynamics for the corresponding solutions and examine the stability of these black holes in context of canonical ensemble. We continue with the calculation of the optical features of this kind of black holes such as the shadow geometrical shape, the energy emission rate and the deflection angle. Taking into account these optical quantities, we analysis the effective role of the parameters of models on them. We also employ the correspondence between the quasinormal modes in the eikonal limit and shadow radius to study the scalar field perturbations in these backgrounds. Finally, we take advantage of the WKB method and investigate how the quasinormal modes will be disturbed for massive particles.

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Hawking evaporation of black holes in massive gravity

Cited by 23 publications

References 42 publications

Greybody factor for black holes in dRGT massive gravity

Greybody factor for black holes in dRGT massive gravity

A critical assessment of black hole solutions with a linear term in their redshift function

Three-dimensional AdS black holes in massive-power-Maxwell theory

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