Abstract
In the present paper, we treat the problem of the existence of quark stars (QSs) for selected homogeneous and unpaired charge-neutral 3-flavor interacting quark matter with O(ms4) corrections equations of state (EoS). Using the EoS combined with the Tolmann-Oppenheimer-Volkoff (TOV) structure equations, the properties of stars are explored by obtaining their mass-radius relations. All calculations are carried out within the framework of the R-squared gravity defined by f(R)=R+aR2. Our main goal is to discuss the effect for a wide range of the R-squared gravity parameter, a, on the mass-radius and the mass-central mass density (M−ϵc) relation of QSs. Furthermore, we investigate the dynamical stability condition for those stars, and we show that their dynamical stability depends on the anisotropic parameters B⊥ and a4⊥ coming from the respective EoS. In such a scenario our results provide circumstantial evidence in favor of super-massive pulsars.
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