Anisotropic star with a linear equation of state (EOS)

Abstract

A family of solutions defining the interior of a static, spherically symmetric, compact anisotropic star is described by considering a new form of the equation of state (EOS). The analytic solution is derived by using the Finch and Skea ansatz for the metric potential g_rr, which has a clear geometric interpretation for the related background spacetime. The model parameters are fixed by smooth matching of the interior solution to the Schwarzschild exterior metric over the bounding surface of the compact star, together with the requirement that the radial pressure vanishes at the boundary. Data available for the pulsar 4U1802030 has been utilized to analyze the physical viability of the developed model. The model is shown to be stable.

Figures (11)

• Figure 1: Variation of density against radius $r$.
• Figure 2: Variation of radial pressure against radius $r$.
• Figure 3: Variation of transverse pressure against radius $r$
• Figure 4: Variation of anisotropy against radius $r$.
• Figure 5: Variation of $\frac{dp_r}{d\rho}$ against radius $r$.