2003
DOI: 10.1142/s0218271803003086
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Radiating Spherical Collapse With Heat Flow

Abstract: We present here a simple model of radiative gravitational collapse with radial heat flux which describes qualitatively the stages close to the formation of a superdense cold star. Starting with a static general solution for a cold star, the model can generate solutions for the earlier evolutionary stages. The temporal evolution of the model is specified by solving the junction conditions appropriate for radiating gravitational collapse.

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Cited by 27 publications
(17 citation statements)
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“…where A 0 and B 0 represent a known static solution (See Govender et al 27 for a further discussion of this approach.). It is a simple matter 28 to match (67) to (53) at some inner boundary r 0 .…”
Section: Discussionmentioning
confidence: 99%
“…where A 0 and B 0 represent a known static solution (See Govender et al 27 for a further discussion of this approach.). It is a simple matter 28 to match (67) to (53) at some inner boundary r 0 .…”
Section: Discussionmentioning
confidence: 99%
“…This seems to indicate that our model suits better for radiating compact stars. In favor of this unique result one can go through some supporting literature [94,[96][97][98][99][100]. But this also immediately raises the problem of the energy conservation in the model.…”
Section: Discussionmentioning
confidence: 99%
“…However, the Govender et al [10] model lacked a thermodynamical treatment of the temperature profile. We are in a position to investigate the effect of the perturbation on the temperature profile as the star in this investigation collapses to a final static configuration.…”
Section: S D Maharaj G Govender and M Govendermentioning
confidence: 99%
“…The general framework for such a collapse scenario was first addressed by Govender et al [10] in which a collapsing fluid sphere evolved into the Vaidya-Tikekar superdense star [11].…”
Section: Introductionmentioning
confidence: 99%