Radial stability of anisotropic strange quark stars

TL;DR

This paper investigates how anisotropy affects the stability and maximum mass of strange quark stars using modified equilibrium and oscillation equations with the MIT bag model, revealing conditions for stability and potential implications for other compact objects.

Contribution

It introduces a detailed analysis of anisotropic effects on strange star stability using modified hydrostatic and oscillation equations with two anisotropy models, extending understanding of stability criteria.

Findings

Maximum mass and zero oscillation frequency coincide at the same energy density for $\sigma_s=0$.

Stability regions are determined by $dM/d ho_c>0$ when $p_t(R)$ is fixed.

Results are relevant for stability analysis of other anisotropic compact objects.

Abstract

The influence of the anisotropy in the equilibrium and stability of strange stars is investigated through the numerical solution of the hydrostatic equilibrium equation and the radial oscillation equation, both modified from their original version to include this effect. The strange matter inside the quark stars is described by the MIT bag model equation of state. For the anisotropy two different kinds of local anisotropic $\sigma=p_t-p_r$ are considered, where $p_t$ and $p_r$ are respectively the tangential and the radial pressure: one that is null at the star's surface defined by $p_r(R)=0$, and one that is nonnull on at the surface, namely, $\sigma_s=0$ and $\sigma_s\neq0$. In the case $\sigma_s=0$, the maximum mass value and the zero frequency of oscillation are found at the same central energy density, indicating that the maximum mass marks the onset of the instability. For the case $\sigma_s\neq0$, we show that the maximum mass point and the zero frequency of oscillation coincide in the same central energy density value only in a sequence of equilibrium configurations with the same value of $\sigma_s$. Thus, the stability star regions are determined always by the condition $dM/d\rho_c>0$ only when the tangential pressure is maintained fixed at the star surface's $p_t(R)$. These results are also quite important to analyze the stability of other anisotropic compact objects such as neutron stars, boson stars and gravastars.