Evolution of primordial black holes in Jordan–Brans–Dicke cosmology

Majumdar, A. S.; Gangopadhyay, Debashis; Singh, L. P.

doi:10.1111/j.1365-2966.2008.12925.x

Cited by 24 publications

(18 citation statements)

References 58 publications

(91 reference statements)

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“…Also the accretion of dark energy onto the more general KerrNewman black hole was studied by Madrid et al [29] and Bhadra et al [30]. Till now, several authors [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45] have discussed the accretion of various components of dark energy onto black holes. Recently, there has been a great interest in the study of dark-energy accretion onto a static wormhole [46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Accretions of various types of dark energies onto Morris–Thorne wormhole

Debnath

2014

Eur. Phys. J. C

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In this work, we have studied the accretion of dark energies onto a Morris-Thorne wormhole. Previously, in ref. (González-Díaz, arXiv:hep-th/0607137), it was shown that for quintessence like dark energy, the mass of the wormhole decreases, and for phantom like dark energy, the mass of the wormhole increases. We have assumed two types of dark energy: the variable modified Chaplygin gas and the generalized cosmic Chaplygin gas. We have found the expression of the wormhole mass in both cases. We have found the mass of the wormhole at late universe and this is finite. For our choices of the parameters and the function B(a), these models generate only quintessence dark energy (not phantom) and so the wormhole mass decreases during the evolution of the universe. Next we have assumed the five kinds of parametrizations of well-known dark-energy models. These models generate both quintessence and phantom scenarios i.e., phantom crossing models. So if these dark energies accrete onto the wormhole, then for the quintessence stage, the wormhole mass decreases up to a certain value (a finite value) and then again increases to an infinite value for the phantom stage during whole evolution of the universe. That means that if the five kinds of DE accrete onto a wormhole, the mass of the wormhole decreases up to a certain finite value and then increases in the late stage of the evolution of the universe. We have also shown these results graphically.

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Section: Introductionmentioning

confidence: 99%

Accretions of various types of dark energies onto Morris–Thorne wormhole

Debnath

2014

Eur. Phys. J. C

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“…The lifetime for primordial black holes can be obtained in a scalar-tensor scenario, and is given by [27] t evap = t eq 1 − 5 3…”

Section: Scalar-tensor Cosmologymentioning

confidence: 99%

“…It was shown [27] that for a PBH with M i < (A/B) 1/4 to survive the radiation dominated era, one requires M i ≥ 10 13 M pl . It was shown [27] that for a PBH with M i < (A/B) 1/4 to survive the radiation dominated era, one requires M i ≥ 10 13 M pl .…”

Section: Scalar-tensor Cosmologymentioning

confidence: 99%

Primordial black holes as dark matter

Majumdar¹

2008

AIP Conference Proceedings

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We consider black hole solutions in extended and alternate gravity theories where the geometry of the black hole spacetimes are modified due to extra-dimensional effects. We study the cosmological evolution of primordial black holes in a few such theories. We show that the the phenomenon of accretion of radiation in the radiation dominated era could under certain conditions counterbalance the effect of Hawking evaporation, and this leads to longer lifetime for the black holes in these models. Such black holes could survive till the present era and act as candidates for cold dark matter. We discuss the impact of modified geometry of the black holes on strong gravitational lensing by them, which could be a possible avenue for obtaining observational signatures of extra dimensions.

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“…In recent papers [25,26], it is shown that the accretion of radiation prolongates the lifetime of PBHs. Now one can consider the accretion of radiation for this case also.…”

Section: B Scenario Bmentioning

confidence: 99%

Brans–Dicke Theory and Primordial Black Holes in Early Matter-Dominated Era

Nayak

Singh

2011

Int J Theor Phys

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We show that primordial black holes can be formed in the matter-dominated era with gravity described by the Brans-Dicke theory. Considering an early matter-dominated era between inflation and reheating, we found that the primordial black holes formed during that era evaporate at a quicker rate than those of early radiation-dominated era. Thus, in comparison with latter case, less number of primordial black holes could exist today. Again the constraints on primordial black hole formation tend towards the larger value than their radiation-dominated era counterparts indicating a significant enhancement in the formation of primordial black holes during the matter-dominaed era.PACS numbers: 98.80.-k, 97.60.Lf

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Evolution of primordial black holes in Jordan–Brans–Dicke cosmology

Cited by 24 publications

References 58 publications

Accretions of various types of dark energies onto Morris–Thorne wormhole

Accretions of various types of dark energies onto Morris–Thorne wormhole

Primordial black holes as dark matter

Brans–Dicke Theory and Primordial Black Holes in Early Matter-Dominated Era

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