Causal temperature profiles in horizon-free collapse

Naidu, Nolene F.; Govender, M.

doi:10.1007/s12036-007-0014-6

Cited by 16 publications

(9 citation statements)

References 13 publications

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“…which is the general solution to the resulting form of (24) with the assumption (25) valid for all r. Utilizing solution (26), the Einstein field equations (11)- (14) yield…”

Section: Radiating Euclidean Starsmentioning

confidence: 99%

Thermal Behavior of Euclidean Stars

Govender

Govinder

2010

Int. J. Mod. Phys. D

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A recent study of dissipative collapse considered a contracting sphere in which the areal and proper radii are equal throughout its evolution. The interior spacetime was matched to the exterior Vaidya spacetime which generated a temporal evolution equation at the boundary of the collapsing sphere. We present a solution of the boundary condition which allows the study of the gravitational and thermodynamical behaviour of this particular radiating model.

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“…which is the general solution to the resulting form of (24) with the assumption (25) valid for all r. Utilizing solution (26), the Einstein field equations (11)- (14) yield…”

Section: Radiating Euclidean Starsmentioning

confidence: 99%

Thermal Behavior of Euclidean Stars

Govender

Govinder

2010

Int. J. Mod. Phys. D

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“…It is also well understood that the thermal evolution of the radiating fluid is crucial in any stellar model and the precise role of the relaxation and mean collision time were analysed by Martinez [20], Herrera and Santos [21] and Govender et al [22]. These ideas were further exploited in the more recent work of Naidu et al [23], Naidu and Govender [24] and Maharaj et al [25]. Attempts to model radiating stellar matter with a more realistic form, have been made by imposing either a barotropic or polytropic equation of state for the fluid distribution.…”

Section: Introductionmentioning

confidence: 99%

The effect of a two-fluid atmosphere on relativistic stars

2015

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We model the physical behaviour at the surface of a relativistic radiating star in the strong gravity limit. The spacetime in the interior is taken to be spherically symmetrical and shear-free. The heat conduction in the interior of the star is governed by the geodesic motion of fluid particles and a non-vanishing radially directed heat flux. The local atmosphere in the exterior region is a two-component system consisting of standard pressureless (null) radiation and an additional null fluid with non-zero pressure and constant energy density. We analyse the generalised junction condition for the matter and gravitational variables on the stellar surface and generate an exact solution. We investigate the effect of the exterior energy density on the temporal evolution of the radiating fluid pressure, luminosity, gravitational redshift and mass flow at the boundary of the star. The influence of the density on the rate of gravitational collapse is also probed and the strong, dominant and weak energy conditions are also tested. We show that the presence of the additional null fluid has a significant effect on the dynamical evolution of the star.

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“…The model proposed by Glass (1981) has been extensively studied by Santos (1985) for the junction conditions of a shear-free collapsing spherically symmetric nonadiabatic fluid with radial heat flow. On similar grounds a number of studies have been proposed by de Oliveira et al (1988, 1995), de Oliveira and Santos (1987, Bonnor et al (1989), Kramer (1992), Govender (1997, 2005), Debnath et al (2005), Herrera et al (1998Herrera et al ( , 2004aHerrera et al ( , 2004bHerrera et al ( , 2006Herrera et al ( , 2007Herrera et al ( , 2009), Herrera and Santos (2004), Mitra (2006), Naidu and Govinder (2007); see also references therein. However all such studies differ in their details, all of them describe a collapsing fluid dissipating energy.…”

Section: Introductionmentioning

confidence: 55%

“…The problem of such massive stellar objects was initiated by Vaidya (1951Vaidya ( , 1966, with the extension of Tolman (1939) taking account of outflowing radiation. Some of the authors studied the radiating ball with physically significant solutions in the free streaming case (Tewari 1988, 1994, Pant and Tewari 1990 by solving the modified field equations proposed by , Lindquist et al (1965). However, Herrera et al (1980) presented a new approach to the study of a nonstatic radiating fluid.…”

Section: Introductionmentioning

confidence: 99%

Relativistic model of radiating massive fluid sphere

Pant

Mehta

Tewari

2010

Astrophys Space Sci

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In this paper we present a new class of nonsingular solutions representing time dependent balls of perfect fluid with matter-radiation in general relativity. The solution of the class is suitable for interior modeling of a quasar i.e. a massive radiating star. The interior solution is matched with a zero pressure Vaidya metric. From this solution we constructed a quasar model by assuming the life time of the quasar of ≈10 7 year. We obtained a mass of the quasar of ≈10 9 M θ , linear dimension ≈10 17 km and a rate of emission L ∞ ≈ 10 47 erg/s.

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Causal temperature profiles in horizon-free collapse

Cited by 16 publications

References 13 publications

Thermal Behavior of Euclidean Stars

Thermal Behavior of Euclidean Stars

The effect of a two-fluid atmosphere on relativistic stars

Relativistic model of radiating massive fluid sphere

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