State equations for massless spin fields in static spherical spacetime filled with quintessence

Li, Gu-Qiang; Shi-Fa, Xiao

doi:10.1007/s10714-010-0947-y

Cited by 8 publications

(4 citation statements)

References 22 publications

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“…The influence of quintessence dark energy on spherical symmetric black holes has been obtained by , and the properties of black holes surrounded by quintessence matter have been discussed extensively in the literature (Chen & Wang 2008;Ding et al 2013;Fernando 2012;Gong & Wang 2009;Jamil et al 2015;Kalam et al 2014;Kuriakose & Kuriakose 2008;Li & Xiao 2010;Malakolkalami & Ghaderi 2015a,b;Mandal & Biswas 2015;Thomas et al 2012;Uniyal et al 2015;Varghese & Kuriakose 2009;Kar 2006;Priyabrat Pandey et al 2014Singh et al 2014a,b;Xu et al 2016;. For rotational black holes, the Kerr-Newman-AdS black hole solutions for quintessence dark energy have also been obtained recently (Ghosh 2016;.…”

Section: Introductionmentioning

confidence: 99%

Kerr–anti-de Sitter/de Sitter black hole in perfect fluid dark matter background

Hou

Wang

2018

Class. Quantum Grav.

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We obtain the Kerr-anti-de-sitter (Kerr-AdS) and Kerr-de-sitter (Kerr-dS) black hole (BH) solutions to the Einstein field equation in the perfect fluid dark matter background using the Newman-Janis method and Mathematica package. We discuss in detail the black hole properties and obtain the following main results: (i) From the horizon equation g rr = 0, we derive the relation between the perfect fluid dark matter parameter α and the cosmological constant Λ when the cosmological horizon r Λ exists. For Λ = 0, we find that α is in the range 0 < α < 2M for α > 0 and −7.18M < α < 0 for α < 0. For positive cosmological constant Λ (Kerr-AdS BH), α max decreases if α > 0, and α min increases if α < 0. For negative cosmological constant −Λ (Kerr-dS BH), α max increases if α > 0 and α min decreases if α < 0; (ii) An ergosphere exists between the event horizon and the outer static limit surface. The size of the ergosphere evolves oppositely for α > 0 and α < 0, while decreasing with the increasing | α |. When there is sufficient dark matter around the black hole, the black hole spacetime changes remarkably; (iii) The singularity of these black holes is the same as that of rotational black holes. In addition, we study the geodesic motion using the Hamilton-Jacobi formalism and find that when α is in the above ranges for Λ = 0, stable orbits exist. Furthermore, the rotational velocity of the black hole in the equatorial plane has different behaviour for different α and the black hole spin a. It is asymptotically flat and independent of α if α > 0 while is asymptotically flat only when α is close to zero if α < 0. We anticipate that Kerr-Ads/dS black holes could exist in the universe and our future work will focus on the observational effects of the perfect fluid dark matter on these black holes.

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Section: Introductionmentioning

confidence: 99%

Kerr–anti-de Sitter/de Sitter black hole in perfect fluid dark matter background

Hou

Wang

2018

Class. Quantum Grav.

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“…Hence, for a broad analysis of the Kiselev metric and for this choice of metric parameter we refer to Appendix A and for example, to 49,[51][52][53][54][55][56][57][58][59][60][61][62]. In Appendix A we proceed with the analysis of the spacetime properties within this choice of the α parameter and spin a > 0 by considering the ergosufaces and detailing the conditions for the horizons existence, then examining the extreme BH Kiselev spacetimes.…”

Section: The Kiselev Spacetimesmentioning

confidence: 99%

“…Optical effects, as lensing, or spin precession have been also explored to distinguish BH from naked singularity (NS) solutions in Kiselev spacetimes -see [52][53][54][55][56][57][58][59][60][61]. A study of the state equations for massless spin fields in static spherical spacetime filled with quintessence (Kiselev spacetime) is in [62].…”

Section: Introductionmentioning

confidence: 99%

On dark energy effects on the accretion physics around a Kiselev spinning black hole

Pugliese,

Stuchlík

2024

Eur. Phys. J. C

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Kiselev metric in the static and rotating form is widely used to test different aspects of the dark energy (DE) effects. We consider a DE Kiselev spacetime, predicting the reduction to the Kerr black hole (BH) solution under suitable conditions on the DE parameters and in this frame we study the effects of the dark energy on BHs and disks accretion. Elaborating a close comparison with the limiting vacuum Kerr spacetime, we focus on thick accretion disks around the central BH in the Kiselev solution, both co-rotating and counter-rotating with respect the central BH. We examine different aspects of BH accretion energetics by focusing on quantities related to the accretion rates and cusp luminosity, when considered the DE presence, related to the pure Kerr central BH. Our findings show that in these conditions heavy divergences with respect to the vacuum case are expected for the DE metrics. A known effect of the Kiselev metric is to lead to a false estimation the BH spin, we confirm this characteristic from the fluids dynamics analysis. Remarkably our results show that DE is affecting differently the accretion physics, and particularly the accretion rate, according to the fluid rotation orientation with respect to the central spinning attractor, leading in some cases to an under-estimation of the BH spin mass ratio. These contrasting aspects emerging in dependence on the fluids rotational orientation can be a distinguishing general DE feature which could lead to a revised observational paradigm where DE existence is considered.

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“…Li [1,2] used the quantization procedure referred to as the Boulware vacuum state [3] and killing time, t, to investigate the thermodynamic quantities around the Schwarzschild and Reissner-Nordström black hole, and found that their forms differ from those in flat space-times because of the appearance of additional spin-dependent terms. Since then, this method was extended to other Einstein gravity black holes [4][5][6][7][8][9]. However, gravitational interactions were not considered.…”

Section: Introductionmentioning

confidence: 99%

Effects of Quantum Gravity on Thermodynamic Quantities of Gases around a Novel Neutral Four-Dimensional Gauss–Bonnet Black Hole

2023

Universe

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Taking the generalized uncertainty principle (GUP) into account, we apply the corrected state density to investigate the entropy density, energy density, pressure and equation of state for the perfect relativistic gases of massless particles with an arbitrary spin of s ≤ 2 surrounding a new four-dimensional neutral Gauss–Bonnet black hole. The modifications of these thermodynamic quantities by the gravity correction factor and particle spin are shown, and the expressions have completely different forms from those in flat space-times. For example, the energy density is not proportional to the fourth power of the temperature. In other words, the energy density differs from that of blackbody radiation. The quantum gravity effects reduce these quantities and are proportional to the gravity correction factor. The result that the equation of state is not zero is compatible with the non-vanishing trace of the stress tensor.

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State equations for massless spin fields in static spherical spacetime filled with quintessence

Cited by 8 publications

References 22 publications

Kerr–anti-de Sitter/de Sitter black hole in perfect fluid dark matter background

Kerr–anti-de Sitter/de Sitter black hole in perfect fluid dark matter background

On dark energy effects on the accretion physics around a Kiselev spinning black hole

Effects of Quantum Gravity on Thermodynamic Quantities of Gases around a Novel Neutral Four-Dimensional Gauss–Bonnet Black Hole

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