A different approach to anisotropic spherical collapse with shear and heat radiation

Abstract

In order to study the type of collapse, mentioned in the title, we introduce a physically meaningful object, called the horizon function. It directly enters the expressions for many of the stellar characteristics. The main junction equation, which governs the collapse, transforms into a Riccati equation with simple coefficients for the horizon function. We integrate this equation in the geodesic case. The same is done in the general case when one or another of the coefficients vanish. It is shown how to build classes of star models in this formulation of the problem and simple solutions are given.

15 pages, to appear in Int.J.Mod.Phys.D

References in corpus (12)

• Nonadiabatic charged spherical gravitational collapse
• Shearing Expansion-free Spherical Anisotropic Fluid Evolution
• Some analytical models of radiating collapsing spheres
• Collapsing shear-free perfect fluid spheres with heat flow
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Cited by in corpus (7)

• Definition of complexity for dynamical spherically symmetric dissipative self-gravitating fluid distributions
• Quasi-homologous evolution of self-gravitating systems with vanishing complexity factor
• Radiating stars with exponential Lie symmetries
• Riccati equations for bounded radiating systems
• On Properties of Expansion-free Dynamical Stars
• Lie Symmetries, Painlevé analysis and global dynamics for the temporal equation of radiating stars
• Non-existence of expansion-free dynamical stars with rotation and spatial twist