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The role of shear in dissipative gravitational collapse
In this paper we investigate the physics of a radiating star undergoing
dissipative collapse in the form of a radial heat flux. Our treatment clearly
demonstrates how the presence of shear affects the collapse process; we are in
a position to contrast the physical features of the collapsing sphere in the
presence of shear with the shear-free case. By employing a causal heat
transport equation of the Maxwell-Cattaneo form we show that the shear leads to
an enhancement of the core temperature thus emphasizing that relaxational
effects cannot be ignored when the star leaves hydrostatic equilibrium.Comment: 15 pages, To appear in Int. J. Mod. Phys.
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