Anisotropic compact stars: Constraining model parameters to account for physical features of tidal Love numbers

Abstract

In this paper, we develop a new class of models for a compact star with anisotropic stresses inside the matter distribution. By assuming a linear equation of state for the anisotropic matter composition of the star we solve the Einstein field equations. In our approach, for the interior solutions we use a particular form of the ansatz for the metric function g rr . The exterior solution is assumed as Schwarzschild metric and is joined with the interior metric obtained across the boundary of the star. These matching of the metrices along with the condition of the vanishing radial pressure at the boundary lead us to determine the model parameters. The physical acceptability of the solutions has verified by making use of the current estimated data available from the pulsar 4U 1608−52. Thereafter, assuming anisotropy due to tidal effects we calculate the Love numbers from our model and compare the results with the observed compact stars, viz.

Wormhole solutions in f(R) gravity

“…∆ = 0 which will be responsible for tidal deformation in the wormhole system and thus may have stability problem. However, this issue of possible calculation of tidal effect via Love numbers can be tackled in a future project 84 .…”

New anisotropic star solutions in mimetic gravity

“…Let us examine whether our solutions satisfy the above necessary physical conditions. In order to proceed we need to give numerical values to the model parameters c 1 , c 2 and k. This will be obtained by using as input values the mass and radius of the pulsar 4U 1608-52, estimated respectively as M = 1.57 +0.3 −0.29 M ⊙ and l = 9.8 ± 1.8 km [105][106][107]. Inserting these values into (3.21)-(3.23), we find where (c 1 ) 1 s−2 has units of km, c 2 is dimensionless and k has units of km 2 .…”