Collapse of a charged radiating star with shear

Maharaj, S. D.; Govender, M.

doi:10.1007/s12043-000-0117-y

Cited by 48 publications

(28 citation statements)

References 30 publications

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“…This is a necessary condition that ensures continuity of the momentum flux across the boundary of the radiating star. The Santos junction conditions have been generalised to include shear [5,6], the cosmological constant as well as the electromagnetic field [7,8]. Since 1985 there has been a concerted effort in generating exact models of dissipative collapse with Herrera and co-workers establishing many of the fundamental results in terms of stability, energy conditions and thermodynamics of these models [9][10][11][12][13][14].…”

Section: Introductionmentioning

confidence: 99%

Radiating star with a time-dependent Karmarkar condition

Naidu

Govender

2018

Eur. Phys. J. C

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In this paper we employ the Karmarkar condition (Proc Indian Acad Sci A 27:56, 1948) to model a spherically symmetric radiating star undergoing dissipative gravitational collapse in the form of a radial heat flux. A particular solution of the boundary condition renders the Karmarkar condition independent of time which allows us to fully specify the spatial behaviour of the gravitational potentials. The interior solution is smoothly matched to Vaidya's outgoing solution across a time-like hypersurface which yields the temporal behaviour of the model. Physical analysis of the matter and thermodynamical variables show that the model is wellbehaved.

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Section: Introductionmentioning

confidence: 99%

Radiating star with a time-dependent Karmarkar condition

Naidu

Govender

2018

Eur. Phys. J. C

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“…In the investigations of de Oliveira et al [9] and Maharaj and Govender [10], the Santos junction conditions were generalised to include the effects of an electromagnetic field and shearing anisotropic stresses during dissipative stellar collapse. More recently, analytical models for shear-free nonadiabatic collapse in the presence of electric charge were obtained by Pinheiro and Chan [11].…”

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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“…Subsequently, many models of shear-free radiative collapse were developed and the physical viability of these models were studied in great detail 7,8,9,10,11 . These junction conditions were later generalised to include pressure anisotropy 12 and the electromagnetic field 13 . There are a few exact solutions to the Einstein field equations for a bounded shearing matter configuration.…”

Section: Introductionmentioning

confidence: 99%

Thermal Evolution of a Radiating Anisotropic Star With Shear

Naidu

Govender

Govinder

2006

Int. J. Mod. Phys. D

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We study the effects of pressure anisotropy and heat dissipation in a spherically symmetric radiating star undergoing gravitational collapse. An exact solution of the Einstein field equations is presented in which the model has a Friedmann-like limit when the heat flux vanishes. The behaviour of the temperature profile of the evolving star is investigated within the framework of causal thermodynamics. In particular, we show that there are significant differences between the relaxation time for the heat flux and the relaxation time for the shear stress.

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Collapse of a charged radiating star with shear

Cited by 48 publications

References 30 publications

Radiating star with a time-dependent Karmarkar condition

Radiating star with a time-dependent Karmarkar condition

The effect of a two-fluid atmosphere on relativistic stars

Thermal Evolution of a Radiating Anisotropic Star With Shear

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