The role of shear in dissipative gravitational collapse

Abstract

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.

arXiv comment15 pages, To appear in Int. J. Mod. Phys. D

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Cited by in corpus (9)

• Shear-free axially symmetric dissipative fluids
• A different approach to anisotropic spherical collapse with shear and heat radiation
• Generalized Euclidean stars with equation of state
• Radiating fluid sphere immersed in an anisotropic atmosphere
• A Vaidya-type spacetime with no singularities
• Gravitational collapse for a radiating anisotropic fluid
• Axially Symmetric Shear-free Fluids in $f(R,T)$ Gravity
• A regular version of the extremal RN spacetime
• Stability and Horizon Formation during Dissipative Collapse