scholarly journals Thermodynamics of a Bardeen black hole in noncommutative space

2011 ◽  
Vol 89 (10) ◽  
pp. 1027-1033 ◽  
Author(s):  
M. Sharif ◽  
Wajiha Javed
Keyword(s):  
Black Hole ◽  
Energy Distribution ◽  
Black Hole Solution ◽  
Mass Function ◽  
Suitable Choice ◽  
Noncommutative Space ◽  
Black Hole Mass ◽  
Regular Black Hole ◽  
Commutative Space ◽  
Space Noncommutativity

In this paper, we examine the effects of space noncommutativity on the thermodynamics of a Bardeen charged regular black hole. For a suitable choice of sets of parameters, the behavior of the singularity, horizon, mass function, black hole mass, temperature, entropy and its differential, area, and energy distribution of the Bardeen solution have been discussed graphically for both noncommutative and commutative spaces. Graphs show that the commutative coordinates extrapolate all such quantities (except temperature) for a given set of parameters. It is interesting to mention here that these sets of parameters provide the singularity (essential for rh > 0) and horizon (f(rh) = 0 for rh > 0) for the black hole solution in noncommutative space, while for commutative space no such quantity exists.

scholarly journals Energy Distribution of a Regular Black Hole Solution in Einstein-Nonlinear Electrodynamics

2015 ◽  
Vol 2015 ◽  
pp. 1-12 ◽  
Author(s):  
I. Radinschi ◽  
F. Rahaman ◽  
Th. Grammenos ◽  
A. Spanou ◽  
Sayeedul Islam
Keyword(s):  
Black Hole ◽  
Positive Integer ◽  
Energy Distribution ◽  
Black Hole Solution ◽  
Mass Function ◽  
Nonlinear Electrodynamics ◽  
Radial Coordinate ◽  
Regular Black Hole ◽  
Limiting Behavior ◽  
Special Case

A study about the energy momentum of a new four-dimensional spherically symmetric, static and charged, regular black hole solution developed in the context of general relativity coupled to nonlinear electrodynamics is presented. Asymptotically, this new black hole solution behaves as the Reissner-Nordström solution only for the particular valueμ=4, whereμis a positive integer parameter appearing in the mass function of the solution. The calculations are performed by use of the Einstein, Landau-Lifshitz, Weinberg, and Møller energy momentum complexes. In all the aforementioned prescriptions, the expressions for the energy of the gravitating system considered depend on the massMof the black hole, its chargeq, a positive integerα, and the radial coordinater. In all these pseudotensorial prescriptions, the momenta are found to vanish, while the Landau-Lifshitz and Weinberg prescriptions give the same result for the energy distribution. In addition, the limiting behavior of the energy for the casesr→∞,r→0, andq=0is studied. The special caseμ=4andα=3is also examined. We conclude that the Einstein and Møller energy momentum complexes can be considered as the most reliable tools for the study of the energy momentum localization of a gravitating system.

scholarly journals Energy-Momentum for a Charged Nonsingular Black Hole Solution with a Nonlinear Mass Function

2017 ◽  
Vol 2017 ◽  
pp. 1-10 ◽  
Author(s):  
Irina Radinschi ◽  
Theophanes Grammenos ◽  
Farook Rahaman ◽  
Andromahi Spanou ◽  
Sayeedul Islam ◽  
...  
Keyword(s):  
Black Hole ◽  
Energy Distribution ◽  
Black Hole Solution ◽  
Mass Function ◽  
Nonlinear Electrodynamics ◽  
Logistic Distribution ◽  
Radial Coordinate ◽  
Additional Parameter ◽  
Limiting Behavior ◽  
Energy And Momentum

The energy-momentum of a new four-dimensional, charged, spherically symmetric, and nonsingular black hole solution constructed in the context of general relativity coupled to a theory of nonlinear electrodynamics is investigated, whereby the nonlinear mass function is inspired by the probability density function of the continuous logistic distribution. The energy and momentum distributions are calculated by use of the Einstein, Landau-Lifshitz, Weinberg, and Møller energy-momentum complexes. In all these prescriptions, it is found that the energy distribution depends on the mass M and the charge q of the black hole, an additional parameter β coming from the gravitational background considered, and the radial coordinate r. Further, the Landau-Lifshitz and Weinberg prescriptions yield the same result for the energy, while, in all the aforesaid prescriptions, all the momenta vanish. We also focus on the study of the limiting behavior of the energy for different values of the radial coordinate, the parameter β, and the charge q. Finally, it is pointed out that, for r→∞ and q=0, all the energy-momentum complexes yield the same expression for the energy distribution as in the case of the Schwarzschild black hole solution.

scholarly journals Einstein and Møller Energy-Momentum Distributions for the Static Regular Simpson–Visser Space-Time

Symmetry ◽  
2021 ◽  
Vol 13 (9) ◽  
pp. 1622
Author(s):  
Irina Radinschi ◽  
Theophanes Grammenos ◽  
Gargee Chakraborty ◽  
Surajit Chattopadhyay ◽  
Marius Mihai Cazacu
Keyword(s):  
Black Hole ◽  
Energy Distribution ◽  
Gravitational Lensing ◽  
Black Hole Solution ◽  
Radial Coordinate ◽  
Spherically Symmetric ◽  
Wormhole Solution ◽  
Schwarzschild Black Hole ◽  
Regular Black Hole ◽  
Momentum Distributions

Energy-momentum localization for the four-dimensional static and spherically symmetric, regular Simpson–Visser black hole solution is studied by use of the Einstein and Møller energy-momentum complexes. According to the particular values of the parameter of the metric, the static Simpson–Visser solution can possibly describe the Schwarzschild black hole solution, a regular black hole solution with a one-way spacelike throat, a one-way wormhole solution with an extremal null throat, or a traversable wormhole solution of the Morris–Thorne type. In both prescriptions it is found that all the momenta vanish, and the energy distribution depends on the mass m, the radial coordinate r, and the parameter a of the Simpson–Visser metric. Several limiting cases of the results obtained are discussed, while the possibility of astrophysically relevant applications to gravitational lensing issues is pointed out.

scholarly journals OPTICAL THERMONUCLEAR TRANSIENTS FROM TIDAL COMPRESSION OF WHITE DWARFS AS TRACERS OF THE LOW END OF THE MASSIVE BLACK HOLE MASS FUNCTION

2016 ◽  
Vol 819 (1) ◽  
pp. 3 ◽  
Author(s):  
Morgan MacLeod ◽  
James Guillochon ◽  
Enrico Ramirez-Ruiz ◽  
Daniel Kasen ◽  
Stephan Rosswog
Keyword(s):  
Black Hole ◽  
White Dwarfs ◽  
Mass Function ◽  
Black Hole Mass ◽  
Massive Black Hole

scholarly journals Constraining the stellar mass function from the deficiency of tidal disruption flares in the nuclei of massive galaxies

2019 ◽  
Vol 485 (3) ◽  
pp. 4413-4422 ◽  
Author(s):  
Daniel J D’Orazio ◽  
Abraham Loeb ◽  
James Guillochon
Keyword(s):  
Black Hole ◽  
Mass Function ◽  
Stellar Mass ◽  
High Mass ◽  
Black Hole Mass ◽  
Tidal Disruption ◽  
Massive Black Hole ◽  
Massive Black Holes ◽  
Massive Galaxies ◽  
O 10

ABSTRACT The rate of tidal disruption flares (TDFs) per mass of the disrupting black hole encodes information on the present-day mass function (PDMF) of stars in the clusters surrounding super massive black holes. We explore how the shape of the TDF rate with black hole mass can constrain the PDMF, with only weak dependence on black hole spin. We show that existing data can marginally constrain the minimum and maximum masses of stars in the cluster, and the high-mass end of the PDMF slope, as well as the overall TDF rate. With $\mathcal {O}(100)$ TDFs expected to be identified with the Zwicky Transient Facility, the overall rate can be highly constrained, but still with only marginal constraints on the PDMF. However, if ${\lesssim } 10 {{\ \rm per\ cent}}$ of the TDFs expected to be found by LSST over a decade ($\mathcal {O}(10^3)$ TDFs) are identified, then precise and accurate estimates can be made for the minimum stellar mass (within a factor of 2) and the average slope of the high-mass PDMF (to within $\mathcal {O}(10{{\ \rm per\ cent}})$) in nuclear star clusters. This technique could be adapted in the future to probe, in addition to the PDMF, the local black hole mass function and possibly the massive black hole binary population.

scholarly journals On the Energy of a Non-Singular Black Hole Solution Satisfying the Weak Energy Condition

Universe ◽  
2020 ◽  
Vol 6 (10) ◽  
pp. 169
Author(s):  
Irina Radinschi ◽  
Theophanes Grammenos ◽  
Farook Rahaman ◽  
Marius-Mihai Cazacu ◽  
Andromahi Spanou ◽  
...  
Keyword(s):  
General Relativity ◽  
Black Hole ◽  
Energy Distribution ◽  
Black Hole Solution ◽  
Energy Condition ◽  
Weak Energy Condition ◽  
Radial Coordinate ◽  
Spherically Symmetric ◽  
Comparison Of The Results ◽  
Two Parameters

The energy-momentum localization for a new four-dimensional and spherically symmetric, charged black hole solution that through a coupling of general relativity with non-linear electrodynamics is everywhere non-singular while it satisfies the weak energy condition, is investigated. The Einstein and Møller energy-momentum complexes have been employed in order to calculate the energy distribution and the momenta for the aforesaid solution. It is found that the energy distribution depends explicitly on the mass and the charge of the black hole, on two parameters arising from the space-time geometry considered, and on the radial coordinate. Further, in both prescriptions all the momenta vanish. In addition, a comparison of the results obtained by the two energy-momentum complexes is made, whereby some limiting and particular cases are pointed out.

scholarly journals The Distribution and Evolution of Black Hole Mass in Broad Line Quasars

2009 ◽  
Vol 5 (S267) ◽  
pp. 263-263
Author(s):  
Brandon C. Kelly ◽  
Marianne Vestergaard ◽  
Xiaohui Fan ◽  
Lars Hernquist ◽  
Philip Hopkins ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Mass Function ◽  
Sloan Digital Sky Survey ◽  
Broad Line ◽  
Black Hole Mass ◽  
Sky Survey ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Eddington Limit

We present the first estimate of the black hole mass function (BHMF) of broad-line quasars (BLQSOs) that self-consistently corrects for incompleteness and the statistical uncertainty in the mass estimates, based on a sample of 9886 quasars at 1 < z < 4.5 drawn from the Sloan Digital Sky Survey. We find evidence for “cosmic downsizing” of black holes in BLQSOs, where the peak in their number density shifts to higher redshift with increasing black hole mass. We estimate the lifetime of the BLQSO phase to be 70 ± 5 Myr for supermassive black holes (SMBHs) at z = 1 with a mass of MBH = 109M⊙, and we constrain the maximum mass of a black hole in a BLQSO to be ~ 1010M⊙. We find that most BLQSOs are not radiating at or near the Eddington limit. Our results are consistent with models for self-regulated black hole growth, where the BLQSO phase occurs at the end of a fueling event when black hole feedback unbinds the accreting gas.

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