2015
DOI: 10.1103/physrevd.91.083011
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Abstract: We explore thick accretion disks around rotating attractors. We detail the configurations analysing the fluid angular momentum and finally providing a characterization of the disk morphology and different possible topologies. Investigating the properties of orbiting disks, a classification of attractors, possibly identifiable in terms of their spin-mass ratio, is introduced; then an attempt to characterize dynamically a series of different disk topologies is discussed, showing that some of the toroidal configu… Show more

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Cited by 31 publications
(103 citation statements)
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References 63 publications
(145 reference statements)
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“…The tori are governed by "Boyer's condition" of the analytic theory of equilibrium configurations of rotating perfect fluids [65]. The toroidal structures of orbiting barotropic perfect fluid are determined by an effective potential reflecting the spacetime geometry, and the centrifugal force component through the distribution of the specific angular momentum (r) of the orbiting fluid - [26,66,67,64,68,69,70,71,72,73,74,56,75]. The entropy is constant along the flow and, according to the von Zeipel condition, the surfaces of constant angular velocity Ω and of constant specific angular momentum coincide [76,77,78] (this implies in particular that the rotation law = (Ω) is independent of the equation of state [64,79]).…”
Section: Introductionmentioning
confidence: 99%
“…The tori are governed by "Boyer's condition" of the analytic theory of equilibrium configurations of rotating perfect fluids [65]. The toroidal structures of orbiting barotropic perfect fluid are determined by an effective potential reflecting the spacetime geometry, and the centrifugal force component through the distribution of the specific angular momentum (r) of the orbiting fluid - [26,66,67,64,68,69,70,71,72,73,74,56,75]. The entropy is constant along the flow and, according to the von Zeipel condition, the surfaces of constant angular velocity Ω and of constant specific angular momentum coincide [76,77,78] (this implies in particular that the rotation law = (Ω) is independent of the equation of state [64,79]).…”
Section: Introductionmentioning
confidence: 99%
“…This is a clear indication of the observational differences between black holes and naked singularities. The allowed values for the frequencies are bounded by the limiting value ω 0 = M/a; for a broader discussion on the role of the dimensionless spin parameter a/M in Kerr geometries, see also [96]. 9 Moreover, for a given value of ω ± , the corresponding radius is located at a certain distance from the source, depending on the value of the rotational parameter a.…”
Section: The Frequencies ω ±mentioning
confidence: 99%
“…When we consider the principal null congruence γ ± ≡ ±∂ r + Δ −1Ṽ , the angular momentum L = aσ 2 , that is,¯ = 1 (and E = +1, in proper units), every principal null geodesic is then characterized by¯ = 1. On the horizon, it is L = E = 0 [96,115]. (31), is marked with a point.…”
Section: The Frequencies ω ±mentioning
confidence: 99%
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