A new anisotropic compact star model having Matese & Whitman mass function

Abstract

Present paper proposed a new singularity free model of anisotropic compact star. The Einstein field equations are solved in closed form by utilizing Matese & Whitman mass function. The model parameters ρ, p r and p t all are well behaved inside the stellar interior and our model satisfies all the required conditions to be physically acceptable. The model given in the present work is compatible with observational data of compact objects like SAX J 1808.4-3658 (SS1), SAX J 1808.4-3658 (SS2) and 4U 1820-30. A particular model of 4U 1820-30 is studied in detail and found that it satisfies all the condition needed for physically acceptable model. The present work is the generalization of Sharma and Ratanpal (Int. J. Mod. Phys. D 22:1350074, 2013) model for compact stars admitting quadratic equation of state.

Effect of electric charge on anisotropic compact stars in conformally symmetric spacetime

“…Dev and Gleiser [16] proposed several exact solutions for anisotropic stars by taking constant density. We have extensively studied the charged and uncharged model of compact stars in some of our earlier works [17][18][19][20][21][22][23][24][25][26]. To find the exact solution, a more systematic approach is to assume conformal symmetry of the space-time.…”

Anisotropic compact star model: a brief study via embedding

“…In literature several number of papers have done by choosing KB ansatz [53, [61][62][63][64][65][66][67][68]. Some compact star models are developed by choosing metric co-efficients e λ along with a reasonable equation of state (relation between the matter density ρ and radial pressure p r ) [69][70][71][72][73][74], by choosing e λ along with p r [75][76][77].…”

Compact stellar model in presence of pressure anisotropy in modified Finch Skea spacetime

“…Now by our previous knowledge of algebra we know that there are 5 2 = 10 possible ways to chose any two unknowns. , Bhar et al (2016a), Bhar & Ratanpal (2016) choose B 2 along with p r , choose ρ along with p r , Murad & Fatema (2015), Thirukkanesh et al (2018) choose A 2 with ∆ to model different compact stars. But a very popular technique is to choose B 2 along with an equation of state (EoS), i.e., a relation between the matter density ρ and radial pressure p r .…”