Dark Matter Effects on the Curvature of Neutron Stars within the new Quarkyonic Model Coupled with Relativistic Mean Field Theory
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arXiv
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| Auteurs principaux: | , , , , |
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| Format: | Preprint |
| Publié: |
2025
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| _version_ | 1866917898311696384 |
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| author | Pattnaik, Jeet Amrit Dey, D. Panda, R. N. Bhuyan, M. Patra, S. K. |
| author_facet | Pattnaik, Jeet Amrit Dey, D. Panda, R. N. Bhuyan, M. Patra, S. K. |
| contents | For the first time, we analyze the impact of dark matter (DM) on the curvature properties of quarkyonic neutron stars (NS) using a hybrid model based on quarkyonic-effective field theory within the relativistic mean-field (E-RMF) framework. This study examines the radial variation of curvature components, including the Ricci scalar ($\cal{R}$), Ricci tensor ($\cal{J}$), Kretschmann scalar ($\cal{K}$), and Weyl tensor ($\cal{W}$), under different DM admixtures. These components offer critical insights into the spacetime geometry and gravitational field strength within the star. The analysis spans canonical mass (1.4 $M_{\odot}$) and maximum mass configurations, varying key parameters such as the transition density ($n_t$) and QCD confinement scale ($Λ_{\rm cs}$), which influence matter transitions and quark confinement. Our results reveal that DM and quarkyonic matter (QM) significantly affect the star's curvature. Central curvature values, particularly $\cal{R}$, $\cal{J}$, and $\cal{K}$, increase with DM due to higher central densities but decrease with stronger QM effects. Stiffer EOSs yield smoother curvature profiles, while softer EOSs influenced by DM redistribute curvature more dynamically. DM softens the EOS, reducing central pressure and compactness, whereas higher $n_t$ values enhance compactness and central pressures. These findings show that dark matter plays a key role in shaping the curvature of quarkyonic neutron stars, offering new insights into compact objects with exotic matter. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2501_11435 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Dark Matter Effects on the Curvature of Neutron Stars within the new Quarkyonic Model Coupled with Relativistic Mean Field Theory Pattnaik, Jeet Amrit Dey, D. Panda, R. N. Bhuyan, M. Patra, S. K. High Energy Astrophysical Phenomena Nuclear Theory For the first time, we analyze the impact of dark matter (DM) on the curvature properties of quarkyonic neutron stars (NS) using a hybrid model based on quarkyonic-effective field theory within the relativistic mean-field (E-RMF) framework. This study examines the radial variation of curvature components, including the Ricci scalar ($\cal{R}$), Ricci tensor ($\cal{J}$), Kretschmann scalar ($\cal{K}$), and Weyl tensor ($\cal{W}$), under different DM admixtures. These components offer critical insights into the spacetime geometry and gravitational field strength within the star. The analysis spans canonical mass (1.4 $M_{\odot}$) and maximum mass configurations, varying key parameters such as the transition density ($n_t$) and QCD confinement scale ($Λ_{\rm cs}$), which influence matter transitions and quark confinement. Our results reveal that DM and quarkyonic matter (QM) significantly affect the star's curvature. Central curvature values, particularly $\cal{R}$, $\cal{J}$, and $\cal{K}$, increase with DM due to higher central densities but decrease with stronger QM effects. Stiffer EOSs yield smoother curvature profiles, while softer EOSs influenced by DM redistribute curvature more dynamically. DM softens the EOS, reducing central pressure and compactness, whereas higher $n_t$ values enhance compactness and central pressures. These findings show that dark matter plays a key role in shaping the curvature of quarkyonic neutron stars, offering new insights into compact objects with exotic matter. |
| title | Dark Matter Effects on the Curvature of Neutron Stars within the new Quarkyonic Model Coupled with Relativistic Mean Field Theory |
| topic | High Energy Astrophysical Phenomena Nuclear Theory |
| url | https://arxiv.org/abs/2501.11435 |