Luminosity of accretion disks in compact objects with a quadrupole

Boshkayev, Kuantay; Konysbayev, Talgar; Kurmanov, Ergali; Luongo, Orlando; Malafarina, Daniele; Quevedo, Hernando

doi:10.1103/physrevd.104.084009

Cited by 23 publications

(11 citation statements)

References 73 publications

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“…The accretion disk luminosity will be therefore determined once the metric is involved as a solution to Einstein's field equations. Since these solutions describe the gravitational field of these BHs [32][33][34], and/or the field outside massive compact objects, such as white dwarfs, neutron stars [35], and more exotic ones 5 , one needs to fix the symmetry underlying the corresponding spacetime [38].…”

Section: Modelling Dark Matter In the Galaxymentioning

confidence: 99%

“…Recent computations of the accretion disk luminosity [33,34,38,39] have shown that a suitable choice for the DM distribution is offered by the exponential sphere density (ESD) [46,47]:…”

Section: Modelling Dark Matter In the Galaxymentioning

confidence: 99%

“…In this appendix, we display the behaviour of the kinematic quantities related to the accretion disk as a function of the radial distance from the central BH. In some recent studies [33,34,38] it was pointed out that the vanishing pressure at the surface radius, r s , requires the condition η(r s ) + λ(r s ) = 0 to hold. However, the numerical solution η n (r s ) emerging from the TOV equations does not satisfies such constraint and, thus, a possible choice is to redefine the function η as…”

Section: Appendix A: Kinematic Quantitiesmentioning

confidence: 99%

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Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

D’Agostino¹,

Giambò²,

Luongo³

2022

Preprint

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In this paper, we consider the hypothesis that fractions of dark matter could be constituted by primordial black holes (PBHs). To test this possibility, we work out the observational properties of a static black hole embedded in the dark matter envelope made of a PBH source. The corresponding modifications of geometry due to such a physical system are investigated, with particular focus on the accretion disk luminosity in spiral galaxies. The impact of the PBH presence is analyzed through modification of the disk luminosity and kinematic quantities. Thus, we discuss possible constraints on the PBH abundance in view of the most recent theoretical bounds. The results of our study indicate that suitable PBH masses are MPBH ∈ [10 6 , 10 12 ]M for PBH fractions fPBH ∈ [10 −3 , 1]. In particular, a comparison with the predictions of the exponential sphere density profile for dark matter suggests that the best-matching configuration is achieved for fPBH = 1 and MPBH = 10 6 M . Consequences with respect to the current knowledge on primordial black hole physics are discussed.

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Section: Modelling Dark Matter In the Galaxymentioning

confidence: 99%

“…Recent computations of the accretion disk luminosity [33,34,38,39] have shown that a suitable choice for the DM distribution is offered by the exponential sphere density (ESD) [46,47]:…”

Section: Modelling Dark Matter In the Galaxymentioning

confidence: 99%

Section: Appendix A: Kinematic Quantitiesmentioning

confidence: 99%

See 1 more Smart Citation

Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

D’Agostino¹,

Giambò²,

Luongo³

2022

Preprint

Self Cite

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“…[16][17][18] for a review, and Refs. [19][20][21][22][23] for the accretion cases). By studying existing observational results, it has been found that PBHs in most mass ranges can only constitute part of DM [17].…”

Section: Introductionmentioning

confidence: 99%

Constraints on primordial black holes with CMB spectral distortions

Yang

2022

Phys. Rev. D

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In the mixed dark matter scenarios consisting of primordial black holes (PBHs) and weakly interacting massive particles (WIMPs), WIMPs can be accreted onto PBHs to form ultracompact minihalos (UCMHs) with a density spike in the early universe. Compared with the classical dark matter halo, UCMHs are formed earlier and have a higher density of center. Since the annihilation rate is proportional to the squared number density of WIMPs, it is expected that WIMPs annihilation within UCMHs is enhanced and has influences on the early universe. Between the time of recombination and matter-radiation equality, the energy released from WIMPs annihilation within UCMHs is injected into the Universe resulting in CMB y-type distortion. We investigate these effects and derive the upper limits on the abundance of PBHs taking advantage of the observational results of Far Infrared Absolute Spectrophotometer (FIRAS). We find that for the WIMPs mass range 1 ≤ mχ ≤ 1000 GeV, the upper limits on the abundance of PBHs are 5 × 10 −3 ≤ ΩPBH ≤ 5 × 10 −2 .

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“…This method led to novel exact solutions, among which the Kerr solution was the simplest case [14]. Despite the fact that the Kerr metric does not have a physically realistic/reasonable interior solution, it is widely used in astronomy and astrophysics to study the physics of black holes and the processes taking place in their vicinity [15][16][17][18][19][20][21][22]. In the present work, we will focus on the approximate Kerr solution and study the motion of test particles in the framework of the adiabatic theory.…”

Section: Introductionmentioning

confidence: 99%

Adiabatic theory in Kerr spacetimes

Boshkayev¹,

Nurbakyt²,

Quevedo³

et al. 2022

Preprint

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We present the main aspects of the adiabatic theory and show that it can be used to study the motion of test particles in general relativity. The theory is based upon the use of vector elements of the orbits and adiabatic invariants. To prove the applicability of the theory in Einstein's gravity theory, we derive a particular representation of the Kerr metric in harmonic coordinates, which allows us to obtain a general formula for the perihelion shift of test particles orbiting on the nonequatorial plane of a rotating central object. We show that the principle of superposition is fulfilled for the individual effects of the gravitational source mass and angular momentum up to the second order. We demonstrate that the adiabatic theory, along with its simplicity, leads to correct results, which in the limiting cases correspond to the ones reported in the literature.

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Luminosity of accretion disks in compact objects with a quadrupole

Cited by 23 publications

References 73 publications

Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

Constraining primordial black holes as a fraction of dark matter through accretion disk luminosity

Constraints on primordial black holes with CMB spectral distortions

Adiabatic theory in Kerr spacetimes

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