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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.
Date January 2011
CreatorsFleming, Darryl.
ContributorsGovender, Megandhren., Maharaj, Sunil D.
Source SetsSouth African National ETD Portal
Detected LanguageEnglish

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