The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach
Abstract 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...
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SpringerOpen
2025-02-01
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| Series: | European Physical Journal C: Particles and Fields |
| Online Access: | https://doi.org/10.1140/epjc/s10052-025-13849-z |
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| author | Sneha Pradhan Piyali Bhar Sanjay Mandal P. K. Sahoo Kazuharu Bamba |
| author_facet | Sneha Pradhan Piyali Bhar Sanjay Mandal P. K. Sahoo Kazuharu Bamba |
| author_sort | Sneha Pradhan |
| collection | DOAJ |
| description | Abstract 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 $$g_{tt}$$ g tt and $$g_{rr}$$ g rr components. Mathematically, this DM-induced deformation is achieved through the CGD method, where the decoupling parameter $$\alpha $$ α 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 $$2.5-2.67 M_{\odot }$$ 2.5 - 2.67 M ⊙ ) and neutron stars (NSTRs) such as EXO 1785-248 [mass= $$1.3_{-0.2}^{+0.2}~M_{\odot }$$ 1 . 3 - 0.2 + 0.2 M ⊙ ], 4U 1608-52 [mass= $$1.74_{-0.14}^{+0.14}~M_{\odot }$$ 1 . 74 - 0.14 + 0.14 M ⊙ ], and PSR J0952-0607 [mass= $$2.35_{-0.17}^{+0.17}~M_{\odot }$$ 2 . 35 - 0.17 + 0.17 M ⊙ ]. 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 $$\alpha $$ α and $$\zeta _1$$ ζ 1 . 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. |
| format | Article |
| id | doaj-art-6cda65f4fb5d4d81a1a5455420d3842b |
| institution | Kabale University |
| issn | 1434-6052 |
| language | English |
| publishDate | 2025-02-01 |
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| series | European Physical Journal C: Particles and Fields |
| spelling | doaj-art-6cda65f4fb5d4d81a1a5455420d3842b2025-02-09T12:51:46ZengSpringerOpenEuropean Physical Journal C: Particles and Fields1434-60522025-02-0185212110.1140/epjc/s10052-025-13849-zThe stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approachSneha Pradhan0Piyali Bhar1Sanjay Mandal2P. K. Sahoo3Kazuharu Bamba4Department of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad CampusDepartment of Mathematics, Government General Degree College SingurFaculty of Symbiotic Systems Science, Fukushima UniversityDepartment of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad CampusFaculty of Symbiotic Systems Science, Fukushima UniversityAbstract 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 $$g_{tt}$$ g tt and $$g_{rr}$$ g rr components. Mathematically, this DM-induced deformation is achieved through the CGD method, where the decoupling parameter $$\alpha $$ α 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 $$2.5-2.67 M_{\odot }$$ 2.5 - 2.67 M ⊙ ) and neutron stars (NSTRs) such as EXO 1785-248 [mass= $$1.3_{-0.2}^{+0.2}~M_{\odot }$$ 1 . 3 - 0.2 + 0.2 M ⊙ ], 4U 1608-52 [mass= $$1.74_{-0.14}^{+0.14}~M_{\odot }$$ 1 . 74 - 0.14 + 0.14 M ⊙ ], and PSR J0952-0607 [mass= $$2.35_{-0.17}^{+0.17}~M_{\odot }$$ 2 . 35 - 0.17 + 0.17 M ⊙ ]. 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 $$\alpha $$ α and $$\zeta _1$$ ζ 1 . 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.https://doi.org/10.1140/epjc/s10052-025-13849-z |
| spellingShingle | Sneha Pradhan Piyali Bhar Sanjay Mandal P. K. Sahoo Kazuharu Bamba The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach European Physical Journal C: Particles and Fields |
| title | The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach |
| title_full | The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach |
| title_fullStr | The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach |
| title_full_unstemmed | The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach |
| title_short | The stability of anisotropic compact stars influenced by dark matter under teleparallel gravity: an extended gravitational deformation approach |
| title_sort | stability of anisotropic compact stars influenced by dark matter under teleparallel gravity an extended gravitational deformation approach |
| url | https://doi.org/10.1140/epjc/s10052-025-13849-z |
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