Anisotropic strange quark stars with a non-linear equation-of-state

Abstract

We obtain an exact analytical solution to Einstein's field equations assuming a non-linear equation-of-state and a particular mass function. Our solution describes the interior of anisotropic color flavor locked strange quark stars. All energy conditions are fulfilled, and therefore the solution obtained here is a realistic solution within General Relativity. The mass-to-radius profile is obtained, and the compactness of the star is computed.

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

“…where G μν is Einstein's tensor, and T μν is the matter stressenergy tensor, which for anisotropic matter takes the form [36,38]…”

“…where we introduce for convenience the mass function m(r ), and d 2 is the line element of the unit two-dimensional sphere. One obtains the Tolman-Oppenheimer-Volkoff equations for a relativistic star with anisotropic matter [36,38]…”

“…where k is a dimensionless numerical factor, while ρ s is the surface energy density. The MIT bag model is characterized by 3 parameters, namely What is more, given that the number of unknown quantities exceeds the number of equations, we may assume a particular density profile ρ(r ) as was done for instance in [36,38]. In our case, we have selected the following density profile:…”

“…Indeed, anisotropies can arise in many scenarios of a dense matter medium, such as phase transitions [33], pion condensation [34], or in presence of type 3A super-fluid [35]. See also [36][37][38][39] as well as [40][41][42] for more recent works on the topic, and references therein. In the latter works relativistic models of anisotropic quark stars were studied, and the energy conditions were shown to be fulfilled.…”

MGD-decoupled black holes, anisotropic fluids and holographic entanglement entropy

“…In addition, anisotropic neutron compact stellar configurations were used to describe the compact objects 4U 1820.30, 4U 1728.34, PSR J0348+0432, RX J185635.3754, PSR 0943+10, the binary pulsar SAX J1808.4-3658 and X-ray binaries Her X-1 and Cen X-3, whose stability was also investigated in the MGD-decoupling context [60,61]. A similar procedure was scrutinized to describe anisotropic colorflavor strange quark stars [62].…”