Speakers
Description
This study investigates the formulation of quarkyonic matter in neutron stars (NS), where both quarks and nucleons are treated as quasi-particles, facilitating a cross-over transition between these phases. Building on early quark matter (QM) theories, this approach aligns with observational constraints on NS properties, such as maximum mass and canonical radius. To enhance the model, we incorporate dark matter (DM), which is gravitationally trapped within the NS. Quarkyonic matter stiffens the equation of state (EOS), while DM softens it, producing results that match observational data on NS macroscopic properties. DM’s effects on NS curvatures are analyzed, with results indicating significant influence on radial curvature profiles, particularly surface curvature in massive stars, while the impact on maximum mass compactness is comparatively minor. In this work, we explore the impact of fermionic DM on NS structure by deriving the EOS under nucleon-quark equilibrium with the relativistic mean-field (RMF) formalism. Using the G3 and IOPB-I parameterizations, we calculate NS properties by varying three parameters: the transition density ($n_t$), QCD confinement scale ($\Lambda_{\rm cs}$), and DM Fermi momentum ($k_f^{\rm DM}$) . Curvature quantities, including the Ricci scalar, Kretschmann scalar, and Weyl tensor, are evaluated to understand spatial variations in curvature across baryonic, quarkyonic, and DM-admixed quarkyonic stars. Results indicate an inverse relationship between EOS stiffness and curvature, while quarkyonic matter increases EOS stiffness and reduces curvature.
| Field of contribution | Phenomenology |
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