Relativistic compact stars with dark matter density profile
Nayan Sarkar, Susmita Sarkar, Ksh. Newton Singh, Farook Rahaman
Abstract
Abstract In this article, we are proposing a model of anisotropic compact star possessing density profile of pseudo-isothermal 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 $$b=12.55$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>b</mml:mi><mml:mo>=</mml:mo><mml:mn>12.55</mml:mn></mml:mrow></mml:math> km and $$B_g=60$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msub><mml:mi>B</mml:mi><mml:mi>g</mml:mi></mml:msub><mml:mo>=</mml:mo><mml:mn>60</mml:mn></mml:mrow></mml:math> MeV/fm $$^3$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msup><mml:mrow/><mml:mn>3</mml:mn></mml:msup></mml:math> .