Gaussian Anisotropy In Strange Quark Stars

Abstract

In this paper for studying the anisotropic strange quark stars, we assume that the radial pressure inside the anisotropic star is a superposition of pressure in an isotropic case plus a Gaussian perturbation term. Considering a proportionality between electric charge density and the density of matter, we solve the TOV equation for different cases numerically. Our results indicate that anisotropy increases the maximum mass $M_{max}$ and also its corresponding radius $R$ for a typical strange quark star. According to our calculations, an anisotropy amplitude of $A=3\times 10^{33}N{m}^{-2}$ with a standard deviation of $\sigma =3\times 10^{3}m$ leads to a neutron star of 1.97$M_{\odot }$. Furthermore, electric charge not only increases the maximum mass and its corresponding radius, but also raises up the anisotropy factor. We can see that the tangential pressure $p_t$ and anisotropy factor $\Delta$ unlike the radial pressure $p_r$ have a maximum on the surface and this maximum increases by adding electric charge effect. However, we show that anisotropy can be more effective than electric charge in rasing maximum mass of strange quark stars.

References in corpus (6)

• Shapiro delay measurement of a two solar mass neutron star
• Electrically Charged Strange Quark Stars
• Thermodynamic consistency, quark mass scaling, and properties of strange matter
• The superflares of soft Gamma-ray repeatres: giant quakes in solid quark stars?
• Anisotropic Pressures in Very Dense Magnetized Matter
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Cited by in corpus (5)

• Compact Anisotropic Models in General Relativity by Gravitational Decoupling
• Charged anisotropic compact objects by gravitational decoupling
• Anisotropic strange stars in the Einstein-Maxwell spacetime
• Geometrically deformed charged anisotropic models in $f(Q,T)$ gravity
• Universal relations for anisotropic interacting quark stars