A spherically symmetric model of anisotropic fluid for strange quark spheres

Abstract

In the present work, we try to find a solution without singularity of Einstein's field equations for the spherically symmetric perfect fluid objects, accurately strange quark spheres, taking into consideration Schwarzschild metric as the outside space-time. An ensemble of inside solutions found on the basis of the simplest linear state equation in the specific form p r = αρ − β. The energy density ρ(r), the radial pressure p r (r) and the tangential pressure p t (r) are devoid of any singularity and exhibit a wellbehaved nature within the generalized anisotropic solution for compact spherical object. The generalized TOV equation is very much preserved inside the system and all energy conditions are excellent. The stability of the matter distribution of our system is checked by the concept of Herrera's cracking and the condition of causality is all around fulfilled for our models. The adiabatic index of our specific configuration is greater than 4/3 in all interior points of the system and the mass-to-radius ratio in our situation is determined also lies within the Buchdahl limit i.e. M/R ≤ 4/3 (≈ 0.444). We explore the physical characteristics based on the analytical model developed for relativistic compact stellar spheres inside the framework of the general theory of relativity. The evaluated mass and radius are in close concurrence with the observational information. We show that various physical characteristics of the known strange spherical object, viz.

Anisotropic Karmarkar stars in f(R, T)-gravity

“…The main objective of this examination are compact spherical objects, for instance, white dwarfs and neutron stars, which depict the end-state of astrophysical progress of main-sequence stars, yet in addition other kinds of stars, for instance, brown and red dwarfs. Besides, along the decades other astrophysical objects have showed in the literature, for instance, hyperon stars [74], quark/hybrid stars [75,76], strange stars [77][78][79][80][81][82][83][84][85][86][87][88][89][90], and significantly more exotic spheres such as boson stars [91].…”

Linear and Riccati equations in generating functions for stellar models in general relativity

“…One may say that then the metric "admits" a perfect fluid as a source. Models with EOS also lead to such relations, see Eqs (31,32,33). Two similar examples are discussed in the next two sections.…”

“…In the literature y is given and a 1 is found from Eq (32) [30], [31], [32], [33], [34], [35], [36], [37], [38], [39]. Due to Eqs (6, 7) one finds quickly y form µ or m. Solutions with LEOS and known µ are given in [40], [41], [42] and [43].…”

“…A special case is the linear EOS (LEOS) pr = aµ − b with constant 0 ≤ a ≤ 1 and the bag constant b ≥ 0, which includes also the case pr = 0. Eq (31) becomes…”

Studies an analytic model of a spherically symmetric compact object in Einsteinian gravity

“…It has as of late demonstrated that the ideal would be to generalize the gravastar picture by corresponding an inside solution matching to a EoS of DE to an outside solution of Schwarzschild at an interface of the junction. Such a spherically symmetrical model ought not to have a horizon and it should deal with a solution of static equilibrium, at some point alluded as a DE object [48,50,[70][71][72][73].…”