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This study employs a holographic model to analyze the physical properties of neutron stars and quark stars by solving the Tolman-Oppenheimer-Volkov equations using analytic equations of state. The researchers investigated key characteristics including gravitational mass, radius, tidal deformabilities, and f-mode oscillations for both types of compact stellar objects. The work demonstrates that holographic equations of state can effectively describe both neutron matter and quark matter while being applicable to astrophysical modeling.
Why it matters
Understanding the properties of compact stars, particularly their oscillation modes and tidal deformabilities, is crucial for interpreting gravitational wave observations from neutron star mergers and for determining the fundamental nature of ultra-dense matter in extreme conditions.
Understand the Science
arXiv:2601.21911v2 Announce Type: replace-cross
Abstract: We use a simple holographic model to study the property of cold and dense neutron stars (NSs) and deconfined QCD matter. With the aim of investigating the global properties of compact stars, such as the total gravitational mass and radius, the equation of states (EOS) of neutron stars and quark stars (QSs) are used to solve the Tolman-Oppenheimer-Volkov (TOV) equations for stellar structure. Additionally, we investigate the tidal deformabilities and $f$-mode oscillation for these two different compact stars. Our main conclusion is that, by using a holographic equation of state, it is possible to obtain neutron matter and quark matter properties and that it is also possible to extend the procedure to astrophysical applications.