2021/11/30 by Nicolás Kovensky, Nicolas Kovensky, Aaron Poole +1 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Asymmetry #Baryon #Black Holes and Theoretical Physics #Formalism (music) #Isospin #Neutron star #Particle physics #Physics #Pulsars and Gravitational Waves Research #Stars #Theoretical physics #astro-ph.HE #hep-ph #hep-th #nucl-th
paper · pdf · doi:10.1103/physrevd.105.034022
19 pages, 12 figures; v2: small correction in Table I, reference added, accepted for publication in PRD; v3: typos in last line of p7 and equation (34b) corrected
openalex publication_date 2022/02/23 · arxiv created 2022/02/28 · arxiv updated 2022/03/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We employ the recently improved description of dense baryonic matter within the Witten-Sakai-Sugimoto model to construct neutron stars. In contrast to previous holographic approaches, the presence of an isospin asymmetry allows us to implement beta equilibrium and electric charge neutrality. As a consequence, we are able to model the crust of the star within the same formalism and compute the location of the crust-core transition dynamically. After showing that a simple pointlike approximation for the baryons fails to satisfy astrophysical constraints, we demonstrate that our improved description does account for neutron stars that meet the current experimental constraints for mass, radius, and tidal deformability. However, we also point out tensions in the parameter fit and large-Nc artifacts and discuss how to potentially resolve them in the future.