2004/04/29 by C. Maieron, M. Baldo, G. F. Burgio +2 · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Color confinement #Condensed matter physics #Dielectric #Equation of state #Gamma-ray bursts and supernovae #Hadron #High-pressure geophysics and materials #Hyperon #Neutron star #Nuclear physics #Nucleon #Particle physics #Phase (matter) #Phase transition #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Quark #Quark model #Solar mass #Stars #Strange matter #astro-ph #hep-ph #nucl-th
paper · pdf · doi:10.1103/physrevd.70.043010
published as Phys.Rev. D70 (2004) 043010 · 11 pages, 5 figures, submitted to Phys. Rev. D
arxiv created 2004/04/29 · openalex publication_date 2004/08/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study the hadron-quark phase transition in the interior of neutron stars (NS). For the hadronic sector, we use a microscopic equation of state (EOS) involving nucleons and hyperons derived within the Brueckner-Bethe-Goldstone many-body theory, with realistic two-body and three-body forces. For the description of quark matter, we employ both the MIT bag model with a density dependent bag constant, and the color dielectric model. We calculate the structure of NS interiors with the EOS comprising both phases, and we find that the NS maximum masses are never larger than 1.6 solar masses, no matter the model chosen for describing the pure quark phase.