Density dependent B parameter of relativistic stars with anisotropy in pseudo-spheroidal space-time

In this paper, the solutions of Einstein–Maxwell Field Equations for relativistic strange quark star in Tolman-IV potential considering MIT bag model EoS $$p=\frac{1}{3}(\rho -4B)$$ p = 1 3 ( ρ - 4 B ) of interior matter in presence of charge in higher dimensions is presented, where B is bag parameter. Here we consider density dependent B as it has more practical application. We note some interesting results. It is observed that interior of a strange quark star may contain bulk stable quarks as a whole having energy per baryon $$E_B<930.4$$ E B < 930.4 MeV/fm$$^3$$ 3 or stable quark matter core enclosed by a thin metastable quark matter layer enveloped by unstable quark matter. It is also found that interior composition depends on the value of space-time dimension (D) and net charge (Q). The model presented in this paper satisfies all the necessary stability and energy conditions for a viable stellar configuration. We also note the maximum mass of stable strange quark star is 1.773 $$M_{\odot }$$ M ⊙ for density dependent B and 1.684 $$M_{\odot }$$ M ⊙ for constant B.

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“…B(ρ)). Following the work of Chattopadhyay and Paul [104], we assume a polynomial relation between p r and ρ as…”

Section: Energy Conditionsmentioning

confidence: 99%

“…4 MeV < E B < 939 MeV) and (iii) unstable (E B > 939 MeV). We consider a polynomial relation [104] between bag parameter B and energy density ρ and find the energy per baryon (E B ) of the system. The variation of E B is studied as a function of ρ.…”

Section: Adiabatic Indexmentioning

confidence: 99%