https://doi.org/10.1140/epjc/s10052-025-13849-z
Regular Article - Theoretical Physics
The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach
1
Department of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad Campus, 500078, Hyderabad, India
2
Department of Mathematics, Government General Degree College Singur, 712409, Hooghly, West Bengal, India
3
Faculty of Symbiotic Systems Science, Fukushima University, 960-1296, Fukushima, Japan
a
pksahoo@hyderabad.bits-pilani.ac.in
Received:
22
November
2024
Accepted:
19
January
2025
Published online:
2
February
2025
In our investigation, we pioneer the development of geometrically deformed strange stars within the framework of teleparallel gravity theory through gravitational decoupling via the complete geometric deformation (CGD) technique. The significant finding is the precise solution for deformed strange star (SS) models achieved through the vanishing complexity factor scenario. Further, we introduce the concept of space-time deformation caused by dark matter (DM) content in DM haloes, leading to perturbations in the metric potentials and
components. Mathematically, this DM-induced deformation is achieved through the CGD method, where the decoupling parameter
governs the extent of DM influence. To validate our findings, we compare our model predictions with observational constraints, including GW190814 (with a mass range of
) and neutron stars (NSTRs) such as EXO 1785-248 [mass=
], 4U 1608-52 [mass=
], and PSR J0952-0607 [mass=
]. Our investigation delves into the stability of the model by considering causality conditions, Herrera’s cracking method, the adiabatic index, and the Harrison–Zeldovich–Novikov criterion. We demonstrate that the developed model mimics a wide range of recently observed pulsars. To emphasize its compatibility, we highlight the predicted mass and radius in tabular form by varying both the parameters
and
. Notably, our findings are consistent with the observation of gravitational waves from the first binary merger event. Furthermore, we compare our results with those obtained for a slow-rotating configuration. In addition to this, we discuss the moment of inertia using the Bejger–Haensel approach in this formulation.
© The Author(s) 2025
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