Bose–Einstein Condensation dark matter models generated by gravitational decoupling
Maurya S.K. Jasim M.K. Errehymy A. Boshkayev K. Mustafa G. Dayanandan B.
December 2024Elsevier B.V.
Physics of the Dark Universe
2024#46
A study on massive compact objects influenced by Bose–Einstein condensation (BEC) dark matter (DM) with a gravitational decoupling approach is presented within the context of f(Q) gravity, assuming a linear form of f(Q). In order to obtain physically valid solutions to the basic field equations of the decoupled systems, we take the Tolman IV potential ansatz for the seed system and the BEC-DM density profile for the new source into consideration. After that, we apply the boundary conditions on the decoupled system with Schwarzschild-de Sitter spacetime as the exterior metric. Eventually, we obtain a complete non-singular solution to the decoupled system, consisting of a strange stellar configuration with a BEC-DM density profile. All the physical properties, such as the effective energy density, pressure along the radial as well as the tangential direction, and anisotropy in the system, are rigorously investigated. Analyzing the stability conditions of the decoupled stellar configuration, we study mass–radius (M−R) relations with observational constraints related to the supermassive compact stars, such as PSR J0740+6620, PSR J2215+5135, GW190814, and GW200210, with observed masses larger than or equal to 2 M⊙. Notably, we examine the influence of DM on constraining the M−R measurements of the observed stars, which satisfy the MIT bag model equation of state as well as the condition of mimicking, i.e., ρθ=ρDM, in the background of f(Q) gravity. Interestingly, any possible conversion of massive compact stars to smaller black holes can be restrained, as the presence of a DM halo in the strange stellar system reduces the maximum mass effectively, as indicated by the M−R curves. This result regarding the maximum mass of the compact star can be associated with the astrophysical data concerning the mass gap of the events GW190814 and GW200210. Specifically, the present model predicts the radius for PSR J0740+6620 as 13.69−0.10+0.09 km, which nearly matches the NICER and XMM-Newton data.
Compact star , Dark matter , Exact solution , Gravitational decoupling
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Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, Nizwa 616
Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, Durban, 4000, South Africa
National Nanotechnology Laboratory of Open Type, Almaty, 050040, Kazakhstan
Al-Farabi Kazakh National University, Al-Farabi avenue 71, Almaty, 050040, Kazakhstan
Institute of Nuclear Physics, Ibragimova, 1, Almaty, 050032, Kazakhstan
Department of Physics, Zhejiang Normal University, Jinhua, 321004
Natural and Medical Sciences Research Centre, University of Nizwa, Nizwa 616
Department of Mathematical and Physical Sciences
Astrophysics Research Centre
National Nanotechnology Laboratory of Open Type
Al-Farabi Kazakh National University
Institute of Nuclear Physics
Department of Physics
Natural and Medical Sciences Research Centre
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