Possible existence of stable compact stars in κ(ℛ,𝒯) gravity

Abstract

In this paper, we present the first interior solutions representing compact stars in [Formula: see text] gravity by solving the modified field equations in isotropic coordinates. Further, we have assumed the metric potentials in Schwarzschild’s form and a few parameters along with the isotropic condition of pressure. For solving, we use specific choice of the running gravitational constant as [Formula: see text]. Once arrived at the reduced field equations, we investigate two solutions with [Formula: see text] and [Formula: see text], where [Formula: see text] denotes here another constant that should not be confused with the speed of light. Then, we investigate each solution by determining the thermodynamics variable viz pressure, density, speed of sound and adiabatic index. We found that these solutions satisfy the Bondi criterion, causality condition and energy conditions. We also found that the [Formula: see text] curves generated from these solutions satisfy the stringent constraints provided by the gravitational wave observations due to the neutron star merger GW 170817.