Compact Q-Stars with q,p-Deformed Fermions

TL;DR

This paper models Q-Star structures, a type of compact, high-density star, using a generalized $q,p$-deformed fermion framework, and explores their properties at various temperatures through numerical solutions of TOV equations.

Contribution

It introduces a novel approach using $q,p$-deformed fermions to model Q-Stars, providing insights into their mass, radius, and temperature-dependent properties.

Findings

Q-Stars can reach up to 13 solar masses and 75 km radius.

Star mass and radius increase as temperature decreases.

Q-Stars become denser at lower temperatures.

Abstract

The Q-Star structures, also called as gray holes with a radius of two times greater than the corresponding Schwarzschild radius of same mass and from the compact neutron star family with a very high density, have been obtained by using a generalization of $q$-deformed fermions with two parameters $q$ and $p$ as the constituents of the star. Because the interaction between particles are controlled by deformation parameters in $q,p$-fermions instead of a complicated interaction Lagrangian, we consider the deformation parameters giving the maximum Q-Star pressure between the interacting particles of stars. The cold and hot Q-Stars in temperatures of $T=0$, $T=40\ \mathrm{MeV}$ and $T=60\ \mathrm{MeV}$ have been investigated from the numerical solutions of TOV equations and it is obtained that the Q-Stars can reach up to $13$ solar mass and $75$ Km radius. Moreover, it is found that the total mass and radius of the star increase when the star gets cool down, and a much denser state is reached.