Relativistic compact stars with dark matter density profile

Abstract

In this article, we are proposing a model of anisotropic compact star possessing density profile of pseudoisothermal dark matter satisfying a linear equation of state (EoS). The stellar system supported by this density profile is physically possible and in equilibrium fulfilling all the energy conditions including the TOV-equation. The solution also satisfies the causality condition, static stability criterion, Abreu's stability and Bondi's criteria. The fulfillment of Rhoades-Ruffini criterion makes our solution more physically viable as well. The M-R curve is plotted for b = 12.55 km and B g = 60 MeV/fm 3 .

A new class of viable and exact solutions of EFEs with Karmarkar conditions: an application to cold star modeling

“…The Karmarkar condition, which needs to be satisfied if the spacetime has to be a class I embedding, has been widely used to generate various stellar models describing anisotropic spheres (Karmarkar 1948). These models have been confirmed to satisfy all the stringent stability and physical tests imposed by the behaviour of the thermodynamic and gravitational variables (Bhar 2019;TellOrtiz et al 2019;Maurya et al 2019a;Jasim et al 2020;Sing et al 2020;Ivano 2020;Sarkar et al 2020). Many of these solutions have been reconciled with observational data of compact objects including strange stars, pulsars and neutron stars (Gedela et al 2018(Gedela et al , 2019aUpreti et al 2020;Fuloria 2017;Pant et al 2020).…”

Strange stars in f(ℛ) gravity palatini formalism and gravitational wave echoes from them

“…Though the relativistic effects for the theory of stellar oscillations are negligible, yet for highly compact objects like neutron stars and strange stars the relativistic limits should be taken into consideration rather than the Newtonian limit. For relativistic cases the system becomes more unstable due to the regenerative effect of pressure [126,127]. However, recently for a stable and relativistic dynamical system, the same condition Γ > 4/3 has been considered in refs.…”

Complexity factor parameterization for traversable wormholes

“…In [14] ways of actually observing wormholes using astrophysical observations is discussed. Some recent articles discusses possible detection of wormholes in the active galactic nuclei [15] and in the bulge of the milky way galaxy [16]. Recently traversable wormholes were constructed in Einstein-Dirac-Maxwell theory without exotic matter [17].…”