Abstract
In the present investigation an exact generalized model for anisotropic compact stars of embedding class one is sought for under general relativistic background. The generic solutions are verified by exploring different physical aspects, viz. energy conditions, mass-radius relation, stability of the models, in connection to their validity. It is observed that the model present here for compact stars is compatible with all these physical tests and thus physically acceptable as far as the compact star candidates $RXJ~1856-37$, $SAX~J~1808.4-3658~(SS1)$ and $SAX~J~1808.4-3658~(SS2)$ are concerned.
Highlights
The studies on anisotropic compact stars have always remained a topic of great interest in relativistic astrophysics
Li et al [19] argued that the object S AX J 1808.43658 with its two variants suggests that S AX J 1808.4-3658 (SS1) and SS2 are “by far the fastest-rotating, lowest-field accretion-driven pulsar known”
It is observed that in Ref. [19] several equations of state (EOS) for rotating neutron star models have been investigated which are not able to reproduce the fast rotation of the object S AX J 1808.4-3658
Summary
The studies on anisotropic compact stars have always remained a topic of great interest in relativistic astrophysics. According to Ruderman [2] for a high density (>1015 gm/cm3) anisotropy is the inherent nature of nuclear matter and their interactions are relativistic In this connection some other work on the anisotropic compact star models can be found in Refs. Though in our study we are unable to explain physical properties like the pulsation or the thermonuclear burst observed in these stars, we can justify some of the basic and important physical features of these ultra-dense compact stars. At this juncture one can argue that a non-rotating model and an extreme fast rotating astrophysical object do not match. Some remarks are made in the concluding section, Sect. 5
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