A GENERAL RELATIVISTIC MODEL FOR SAX J1808.4-3658

Abstract

We discuss the physical applicability of a model for a class of compact stars, employing Vaidya–Tikekar 12 geometry of space–time. It is shown that the model can generate an equation of state (EOS) very similar to the one obtained by earlier workers for SAX J1808.4-3658 (SAX in short), assumed to be a strange star. The stellar configuration, as described by the model, is shown to be stable under radial perturbations. This may explain why the star SAX is known to be very stable compared to other low mass binary X-ray emitters.