Interior solutions of relativistic stars with anisotropic matter in scale-dependent gravity

TL;DR

This paper develops interior solutions for anisotropic relativistic stars within scale-dependent gravity, allowing Newton's constant to vary radially, and analyzes their properties and stability.

Contribution

It introduces a numerical method for modeling anisotropic quark stars with variable Newton's constant in scale-dependent gravity.

Findings

Stars become more massive and compact with decreasing Newton's constant.

Stability criteria and energy conditions are satisfied.

The model provides realistic properties for strange quark stars.

Abstract

We obtain well behaved interior solutions describing hydrostatic equilibrium of anisotropic relativistic stars in scale-dependent gravity, where Newton's constant is allowed to vary with the radial coordinate throughout the star. Assuming i) a linear equation-of-state in the MIT bag model for quark matter, and ii) a certain profile for the energy density, we integrate numerically the generalized structure equations, and we compute the basic properties of the strange quark stars, such as mass, radius and compactness. Finally, we demonstrate that stability criteria as well as the energy conditions are fulfilled. Our results show that a decreasing Newton's constant throughout the objects leads to slightly more massive and more compact stars.