Relativistic model of an anisotropic star with Bose-Einstein dark matter density profile in f (T) gravity

被引：0

作者：

Das, Samprity ^{[1
,2
]}

Rudra, Prabir ^{[3
]}

Chattopadhyay, Surajit ^{[1
]}

机构：

[1] Amity Univ, Dept Math, Major Arterial Rd,Act Area II, Kolkata 700135, India

[2] Shibpur Dinobundhoo Inst Coll, Dept Math, Howrah 711102, W Bengal, India

[3] Asutosh Coll, Dept Math, Kolkata 700026, India

来源：

NUCLEAR PHYSICS B | 2025年 / 1012卷

关键词：

EQUATION-OF-STATE; TIME PHASE-TRANSITION; NEUTRON-STARS; DYNAMICAL INSTABILITY; GALACTIC HALO; GALAXIES; CRACKING; INERTIA; SPHERES;

D O I：

10.1016/j.nuclphysb.2025.116819

中图分类号：

O412 [相对论、场论]; O572.2 [粒子物理学];

学科分类号：

摘要：

This article presents a new model for anisotropic compact stars that are confined to physical dark matter in the background of f(T) teleparallel gravity. The model is based on the equation of state (EoS) of the bag model type and the Bose-Einstein dark matter density profile. The derived solutions meet the energy conditions, the causality conditions, and the required conditions on the stability factor and adiabatic index, indicating that they are physically well-behaved and represent the physical and stable matter configuration. We also determine the maximum mass, surface redshift, and compactness parameter at the surface. Interestingly, all of these numbers fall within the specified range, supporting the physical viability of our proposal. Additionally, the various masses that are derived for varying the model parameter k correspond to five compact, realistic compact objects, including LMC X-4, Her X-1, 4U 1538-52, SAX J1808.4-3658, and Cen X-3. We have also illustrated the radially symmetric profiles of energy density and the moment of inertia for non-rotating stars.

引用

页数：19

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