Braneworld black holes and entropy bounds

Heydarzade, Y.; Hadi, H.; Corda, Christian; Darabi, F.

doi:10.1016/j.physletb.2017.11.061

Cited by 14 publications

(25 citation statements)

References 43 publications

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“…This is because the vacuum solution is just a specific solution which one can not read all the degrees of freedom of the underlying theory from that. For example, in [39] it has been shown that there are vacuum solutions on a 4D brane which are completely different than the vacuum solutions in the GTR. The same happens for the brane solutions with non-vanishing bulk Weyl tensor.…”

Section: : "The Question Which Remains Is How To Construct the Stressmentioning

confidence: 99%

Einstein and Rastall theories of gravitation in comparison

Darabi

Moradpour

Licata³

et al. 2018

Eur. Phys. J. C

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152

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We profit by a recent paper of Visser claiming that Rastall gravity is equivalent to Einstein gravity to compare the two gravitational theories in a general way. Our conclusions are different from Visser's ones. We indeed argue that these two theories are not equivalent. In fact, Rastall theory of gravity is an "open" theory when compared to Einstein general theory of relativity. Thus, it is ready to accept the challenges of observational cosmology and quantum gravity.The framework of extended theories of gravity [1][2][3][4][5] is today considered an useful and popular approach to attempt to solve the important problems of the standard model of cosmology like Dark Energy [6,7] and Dark Matter [8,9]. A key point is that all of the potential alternatives to Einstein's general theory of relativity (GTR) must be viable. This implies that alternative theories must be in agreement with the Einstein's equivalence principle, which has today a strong, unchallengeable empirical evidence [2]. The fundamental consequence is that the alternatives to Einstein gravity must be metric theories [2]. Another important point is that such alternatives must pass the solar system tests. Hence, deviations from the standard GTR must be weak [1,2].Within the framework of extended gravity, one finds the theory proposed by Rastall in 1972 [10], which recently obtained a renewed interest in the literature [11][12][13][14]. This interest is due to some good behavior of the Rastall theory. In fact, on one hand it seems in good agreement with observational data on the Universe age and on the Hubble parameter [15]. On the other hand it may, in principle, provide an alternative description for the matter dominated era with respect to the GTR [16]. Observational data from the helium nucleosynthesis seem also in agreement with Rastall gravity [17]. Based on these observational evidences, there have been some recently studies of the various cosmic eras in the framework of Rastall gravity [18][19][20][21][22]. Other interesting a e-mail: cordac.galilei@gmail.com issues are that Rastall gravity seems to do not suffer from the entropy and age problems of standard cosmology [23] and is consistent with the gravitational lensing phenomena [24,25]. Further interesting works on Rastall gravity are given by [26][27][28][29][30] and references within.Differently from Einstein gravity, Rastall gravity considers a non-divergence-free energy-momentum . A different, but similar theory is the so called Curvature-matter theory of gravity [31][32][33][34][35]. In this theory the matter and geometry are coupled to each other in a non-minimal way [31][32][33][34][35]. Then, the standard energy-momentum conservation law does not work in this case too [31][32][33][34][35].In a recent paper [36], Visser claimed that Rastall gravity is equivalent to Einstein gravity. In this letter, we argue that these two theories are not equivalent instead. Let us see the key points of our interpretation.Rastall did not define a new energy-momentum tensor (EMT) in his origina...

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Section: : "The Question Which Remains Is How To Construct the Stressmentioning

confidence: 99%

Einstein and Rastall theories of gravitation in comparison

Darabi

Moradpour

Licata³

et al. 2018

Eur. Phys. J. C

Self Cite

152

View full text Add to dashboard Cite

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“…where M is original BH mass and n is the BH principal quantum number if the BH is seen as gravitational atom, see e.g., [36][37][38]. We indeed recall that, the intuitive but general belief [36][37][38]: the BHs result in highly excited states representing both the Hydrogen atom and the quasi − thermal emission in quantum gravity, has been shown to be correct, because the Schwarzschild BH results in somewhat similar to the historical semi-classical hydrogen atom introduced by Bohr in 1913, see [36][37][38] for more details. Thus, by using Eqs.…”

Section: Applications To the Excited Bhsmentioning

confidence: 99%

The extended uncertainty principle inspires the Rényi entropy

Moradpour¹,

Corda²,

Ziaie³

et al. 2019

EPL

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We use the extended uncertainty principle (EUP) in order to obtain the Rényi entropy for a black hole (BH). The result implies that the non-extensivity parameter, appeared in the Rényi entropy formalism, may be evaluated from the considerations which lead to EUP. It is also shown that, for excited BHs, the Rényi entropy is a function of the BH principal quantum number, i.e. the BH quantum excited state. Temperature and heat capacity of the excited BHs are also investigated addressing two phases while only one of them can be stable. At this situation, whereas entropy is vanished, temperature may take a non-zero positive minimum value, depending on the value of the non-extensivity parameter. The evaporation time of excited BH has also been studied.

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“…Also, Bousso has achieved the same result for arbitrary dimensions. In another example, the D-bound entropy for the various possible black hole solutions on a four-dimensional brane have been considered in [39] . It is found that the D-bound entropy for this solution is apparently different from that obtained for the four-dimensional black hole solutions.…”

Section: Bekenstein Bound and D-boundmentioning

confidence: 99%

“…This difference is considered as an extra loss of information which comes from the extra dimension, when an extra-dimensional black hole is moved out of the observer's cosmological horizon. The obtained results there also have been considered, by adopting the recent Bohr-like approach to black hole quantum physics for excited black holes [39].…”

Section: Bekenstein Bound and D-boundmentioning

confidence: 99%

D-bound and the Bekenstein bound for the surrounded Vaidya black hole

et al. 2020

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We study the Vaidya black hole surrounded by the exotic quintessence-like, phantom-like and cosmological constant-like fields by means of entropic considerations. Explicitly, we show that for this thermodynamical system, the requirement of the identification of the D-bound and Bekenstein entropy bound can be considered as a thermodynamical criterion by which one can rule out the quintessence-like and phantom-like fields, and prefer the cosmological constant as a viable cosmological field.

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Braneworld black holes and entropy bounds

Cited by 14 publications

References 43 publications

Einstein and Rastall theories of gravitation in comparison

Einstein and Rastall theories of gravitation in comparison

The extended uncertainty principle inspires the Rényi entropy

D-bound and the Bekenstein bound for the surrounded Vaidya black hole

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