NON-ADIABATIC GRAVITATIONAL COLLAPSE OF A SUPERDENSE STAR

摘要: The relativistic equations governing the non-adiabatic shear-free collapse of massive superdense stars in presence dissipative forces producing heat flow background space–times Vaidya–Tikekar ansatz with associated physical three-spaces that have three-spheroidal geometry are formulated. It is shown how system can be used to examine development and progress during subsequent epochs until radiating star becomes a black hole.