Spherically symmetric static matter configurations with vanishing radial pressure

Abstract

We present a new family of spherically symmetric, static solutions of the Einstein field equations in isotropic, comoving coordinates. The radial pressure at each interior point of these models vanishes yet equilibrium is still possible. The constant density Florides solution which describes the gravitational field inside an Einstein cluster is obtained as a special case of our solution-generating method. We show that our solutions can be utilized to model strange star candidates such as Her. X-1, SAX J1808.4-3658(SS2), SAX J1808.4-3658(SS1) and PSR J1614-2230.

Analytical study of anisotropic compact star models

“…The case with p r = 0 was solved completely [64], giving an example of a new solution. The same was done for solutions with LEOS p r = αρ − β [65] and for the Chaplygin EOS [66].…”

A comparative study between EGB gravity and GTR by modeling compact stars

“…Since then, hundreds of exact solutions of the classical field equations describing static fluid spheres have been obtained in which the energy-momentum tensor describing the matter distribution incorporated anisotropy, bulk viscosity, electromagnetic field, scalar field, dark energy, and the cosmological constant. Various techniques ranging from ad hoc assumptions of the gravitational potentials, specifying an equation of state, spacetime symmetry, conformal flatness, to name a few, have been employed to solve the field equations [2][3][4][5][6]. A systematic study of the physical viability of these a e-mail: piyalibhar90@gmail.com b e-mail: megandhreng@dut.ac.za c e-mail: rsharma@associates.iucaa.in solutions have been carried out by Delgaty and Lake [7] who showed that only a few classes of available solutions are capable of describing realistic stellar configurations.…”

Anisotropic static spheres with linear equation of state in isotropic coordinates

“…By assuming a surface density of 2 × 10 14 g.cm −3 , they were able to show that their model describes a super dense quark star with a maximum mass of approximately 1.35 solar masses and a radius of R = 12.58 km. In a recent study of static compact spheres in comoving isotropic coordinates Thirukkanesh et al (2015) presented an intriguing model of a sphere with vanishing radial stresses in the in the interior. They showed that stability is achieved via the tangential stresses and that these models adequately describe strange star candidates such as Her.…”