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## Dissipative gravitating systems.

In this thesis we investigate the effect of shear on radiating stars undergoing gravitational

collapse. The interior spacetime is described by the most general spherically

symmetric line element in the absence of rotation. The energy momentum tensor for

the stellar interior is taken to be an anisotropic

fluid with heat

flux. The thermodynamics

of a relativistic

fluid is reviewed for the Eckart and causal theories. Since the star

is radiating energy to the exterior in the form of a radial heat

flux, the atmosphere is

described by Vaidya's outgoing solution. We provide the matching conditions required

for the continuity of the momentum

flux across the boundary, which determines the

temporal evolution junction conditions for the metric functions. We provide a general

method to obtain shearing solutions of the Einstein field equations describing a radiating,

collapsing sphere. A particular exact solution satisfying the boundary condition

and field equations is found. The validity of this specific model is investigated by employing

a causal heat transport equation which yields the temperature profile within

the stellar core. The energy conditions are studied and yield interesting features of this

particular model which are absent in the shear-free case. / Thesis (M.Sc.)-University of KwaZulu-Natal, Durban, 2011.

Identifer | oai:union.ndltd.org:netd.ac.za/oai:union.ndltd.org:ukzn/oai:http://researchspace.ukzn.ac.za:10413/10923 |

Date | January 2011 |

Creators | Fleming, Darryl. |

Contributors | Govender, Megandhren., Maharaj, Sunil D. |

Source Sets | South African National ETD Portal |

Language | en_ZA |

Detected Language | English |

Type | Thesis |

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