Abstract
We present a number of parametric class of exact solutions of a radiating star and the matching conditions required for the description of physically meaningful fluid. A number of previously known class of solutions have been rediscovered which describe well behaved nature of fluid distributions. The interior matter fluid is shear-free spherically symmetric isotropic and undergoing radial heat flow. The interior metric obeyed all the relevant physical and thermodynamic conditions and matched with Vaidya exterior metric over the boundary. Initially the interior solutions represent a static configuration of perfect fluid which then gradually starts evolving into radiating collapse. The apparent luminosity as observed by the distant observer at rest at infinity and the effective surface temperature are zero in remote past at the instant when collapse begins and at the stage when collapsing configuration reaches the horizon of the black hole.
Highlights
Modern astrophysics opens numerous challenges for researchers to study various aspects of gravitational collapse
The effective surface temperature is zero in the beginning ( f (t ) → 1) and at the stage when collapsing configuration reaches the horizon of the black hole
We have proposed some special solutions of Tewari [20] and a new class of exact solutions corresponding to n = − 5 has been studied in detail
Summary
Modern astrophysics opens numerous challenges for researchers to study various aspects of gravitational collapse. To understand the nature of collapse, it is necessary to form a realistic model, which requires solving non linear differential equations. Santos [10] studied the junction conditions of collapsing spherically symmetric shear-free non-adiabatic fluid with radial heat flow which was based on relativistic models suggested by Glass [11]. Shear-free fluid distributions with radial heat flow are often studied in order to simplify the calculations and allow realistic analytic solutions. In view of the above arguments we present some special solutions of Tewari [20] and demonstrate a detailed study of one such solution in order to construct a realistic model of collapsing radiating star.
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