Anisotropic stars of class one space–time in [formula omitted] gravity under the simplest linear functional of the matter–geometry coupling

Abstract

In the present paper, we have explored the existence of compact structures describing anisotropic matter distributions within the framework of f(R,T) theory, where R is Ricci scalar and T is a trace of energy–momentum tensor. We have chosen f(R,T) as a linear function of R and T, i.e., f(R,T)=R+2χT with χ as matter–geometry coupling constant. We employed the embedding class one technique in order to obtain a full space–time description inside the stellar configuration. After specifying space–time geometry, we determined the complete solution of modified field equations by using the MIT-Bag model equation of state, i.e., pr=13(ρ−4Bg) that describes the strange quark matter distribution inside the stellar system, where Bg represents a bag constant. We checked the physical viability of the solution through different physical tests. Moreover, using observed mass values for the various strange star candidates, we have predicted the exact radii by taking distinct values for χ and Bg. Accordingly, we thoroughly show that with decreasing the value of χ, the stellar systems under examinations become progressively massive and larger in size, transforming them into less dense compact objects. It additionally uncovers that for χ<0 the fR,T gravity arises as an adequate theory for explaining the magnetars, super-Chandrasekhar stars and massive pulsars, which are assumed to be the reason behind the overluminous SNeIa e.g. SN 2003fg, SN 2006gz, SN 2007if, SN 2009dc and remain mostly unexplained in the background of general relativity.