Relativistic compact stars in the Kuchowicz spacetime

Abstract

We present an anisotropic charged analogue of Kuchowicz (1971) solution of the general relativistic field equations in curvature coordinates by using simple form of electric intensity $E$ and pressure anisotropy factor $\Delta$ that involve charge parameter $K$ and anisotropy parameter $\alpha$ respectively. Our solution is well behaved in all respects for all values of $X$ ( $X$ is related to the radius of the star ) lying in the range $0<X\le 0.6$, $\alpha$ lying in the range $0\le \alpha \le 1.3$, $K$ lying in the range $0<K\le 1.75$ and Schwarzschild compactness parameter "$u$" lying in the range $0<u\le 0.338$. Since our solution is well behaved for a wide range of the parameters, we can model many different types of ultra-cold compact stars like quark stars and neutron stars. We present some models of super dense quark stars and neutron stars corresponding to $X=0.2,\alpha =0.2$ and $K=0.5$ for which $u_{max}=0.15$. By assuming surface density ${\rho }_b=4.6888\times 10^{14}g/cc$ the mass and radius are $0.955M_{\odot }$ and $9.439km$ respectively. For ${\rho }_b=2.7\times 10^{14}g/cc$ the mass and radius are $1.259M_{\odot }$ and $12.439km$ respectively and for ${\rho }_b=2\times 10^{14}g/cc$ the mass and radius are $1.463M_{\odot }$ and $14.453km$ respectively. It is also shown that inclusion of more electric charge and anisotropy enhances the static stable configuration under radial perturbations. The $M-R$ graph suggests that the maximum mass of the configuration depends on the surface density {\bf i.e. with the increase of surface density} the maximum mass and corresponding radius decrease. This may be because of existence of exotic matters at higher densities that soften the EoSs.

arXiv comment18 pages, 18 figures, 2 tables. To appear in Ind. J. Phys

References in corpus (12)

• Sound Speeds, Cracking and Stability of Self-Gravitating Anisotropic Compact Objects
• Physical Acceptability of Isolated, Static, Spherically Symmetric, Perfect Fluid Solutions of Einstein's Equations
• All static spherically symmetric anisotropic solutions of Einstein's equations
• Static charged perfect fluid spheres in general relativity
• Nuclear Matter and its Role in Supernovae, Neutron Stars and Compact Object Binary Mergers
• Electric fields at the quark surface of strange stars in the color-flavor locked phase
• Anisotropic Stars II : Stability
• Moments of inertia for neutron and strange stars: limits derived for the Crab pulsar
• Regular models with quadratic equation of state
• Anisotropic Stars: Exact Solutions and Stability
• Constraints on the dense matter EOS from the measurements of PSR J0737-3039A moment of inertia and PSR J0751+1807 mass
• A family of Finch and Skea relativistic stars