Failure of standard thermodynamics in planck scale black hole system

Nozari, Kourosh; Mehdipour, S. Hamid

doi:10.1016/j.chaos.2007.02.018

Cited by 23 publications

(29 citation statements)

References 42 publications

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“…In the delta function case for the scalar curvature , we know that R = 0, r > 0 thus the contribution to the action is zero for all r > 0 ; only the delta function behaviour of the scalar curvature at r = 0 contributes to the action. A detailed study of the nonzero σ modifications of the Hawking temperature, entropy and horizon may be found in [22], [41], [24]. However, as we have seen in the last term of eq-(2.14), when one integrates all over space for any fixed value of σ = ∞ one always gets the same answer in terms of the mass parameter…”

Section: The Euclidean-action-entropy Relation In the Point Mass Schwmentioning

confidence: 88%

“…See [41] and references therein. In [36] a derivation of the logarithmic corrections to the entropy was found based on a generalized p-Loop oscillator in Clifford spaces and an upper limiting Planck temperature was obtained where Black Hole evaporation stops at the Planck scale.…”

Section: 1mentioning

confidence: 99%

“…The authors [41] have obtained the corrections to the area-entropy relation by recurring to the minimal length stringy uncertainty relations by postulating a mass-temperature relation of the form…”

Section: The Euclidean-action-entropy Relation In the Point Mass Schwmentioning

confidence: 99%

“…Concluding, it is in this fashion, by this shifting of horizon locations, how we may avoid the problem of having negative temperatures and negative entropies and the like, because when one tries to go lower than r = 0, one has entered into the white-hole solution region r < 0 of repulsive gravity. Nevertheless this does not mean that non-extensive Tsallis statistics or exotic q-statics in Fractal spacetimes are not relevant in the future as viable solutions to the problem of negative entropy and temperature [41]. The interplay between Non-extensive statistics, Chaos and fractal strings was studied in [55].…”

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confidence: 99%

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The Euclidean gravitational action as black hole entropy, singularities, and spacetime voids

Castro

2008

Journal of Mathematical Physics

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We argue why the static spherically symmetric (SSS) vacuum solutions of Einstein's equations described by the textbook Hilbert metric g µν (r) is not diffeomorphic to the metric g µν (|r|) corresponding to the gravitational field of a point mass delta function source at r = 0. By choosing a judicious radial function R(r) = r + 2G|M |Θ(r) involving the Heaviside step function, one has the correct boundary condition R(r = 0) = 0 , while displacing the horizon from r = 2G|M | to a location arbitrarily close to r = 0 as one desires, r h → 0, where stringy geometry and quantum gravitational effects begin to take place. We solve the field equations due to a delta function point mass source at r = 0, and show that the Euclidean gravitational action (inh units) is precisely equal to the black hole entropy (in Planck area units). This result holds in any dimensions D ≥ 3 . In the Reissner-Nordsrom (massive-charged) and Kerr-Newman black hole case (massive-rotating-charged) we show that the Euclidean action in a bulk domain bounded by the inner and outer horizons is the same as the black hole entropy. When one smears out the point-mass and point-charge delta function distributions by a Gaussian distribution, the areaentropy relation is modified. We postulate why these modifications should furnish the logarithmic corrections (and higher inverse powers of the area) to the entropy of these smeared Black Holes. To finalize, we analyse the Bars-Witten stringy black hole in 1 + 1 dim and its relation to the maximal acceleration principle in phase spaces and Finsler geometries.

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Section: The Euclidean-action-entropy Relation In the Point Mass Schwmentioning

confidence: 88%

Section: 1mentioning

confidence: 99%

Section: The Euclidean-action-entropy Relation In the Point Mass Schwmentioning

confidence: 99%

mentioning

confidence: 99%

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The Euclidean gravitational action as black hole entropy, singularities, and spacetime voids

Castro

2008

Journal of Mathematical Physics

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“…Recently [17], we have reported some results about extraordinary thermodynamical behavior for Planck-scale black hole evaporation, i.e., when M I is less than M 0 , where there is the principal reactiveness to noncommutativity effects and the detailed form of the matter distribution. In this area, some unusual thermodynamical features, e.g., negative entropy, negative temperature, and abnormal heat capacity appeared.…”

Section: Disappearance Of Black Hole Remnantmentioning

confidence: 99%

Hawking radiation as tunneling from a Vaidya black hole in noncommutative gravity

Mehdipour

2010

Phys. Rev. D

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In the context of a noncommutative model of coordinate coherent states, we present a Schwarzschild-like metric for a Vaidya solution instead of the standard Eddington-Finkelstein metric. This leads to the appearance of an exact (t − r) dependent case of the metric. We analyze the resulting metric in three possible causal structures. In this setup, we find a zero remnant mass in the long-time limit, i.e. an instable black hole remnant. We also study the tunneling process across the quantum horizon of such a Vaidya black hole. The tunneling probability including the time-dependent part is obtained by using the tunneling method proposed by Parikh and Wilczek in terms of the noncommutative parameter σ. After that, we calculate the entropy associated to this noncommutative black hole solution. However the corrections are fundamentally trifling; one could respect this as a consequence of quantum inspection at the level of semiclassical quantum gravity.

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Anisotropic compact star model satisfying Karmarkar conditions

Pandya

Thakore

Goti

et al. 2020

Astrophys Space Sci

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A new class of solutions describing the composition of compact stars has been proposed, assuming that the fluid distribution inside the star is anisotropic. This is achieved by assuming the appropriate metric potential and then solving Einstein's field equations using Karmarkar conditions [Karmarkar K. R., Proc. Indian Acad. Sci. 27 (1948) 56] to derive the expressions for star density, the radial and tangential pressures in terms of the constants A, B, a paramter 'a' and the curvature parameter R. The equations thus obtained have been passed through rigorous conditional analysis. It is further shown that the model is physically viable and mathematically well-behaved, fulfilling the requisite conditions viz., regularity condition, strong energy condition, causality condition, etc. Observed star candidates including EXO 1785-248, SMC X-1, SAXJ1808.43658(SS2), HER X-1, 4U 1538-52, Cen X-3 and LMC X-4 were found to conform to a good approximation through the outcome of this model for a=0.5.

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Failure of standard thermodynamics in planck scale black hole system

Cited by 23 publications

References 42 publications

The Euclidean gravitational action as black hole entropy, singularities, and spacetime voids

The Euclidean gravitational action as black hole entropy, singularities, and spacetime voids

Hawking radiation as tunneling from a Vaidya black hole in noncommutative gravity

Anisotropic compact star model satisfying Karmarkar conditions

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