2008/12/19 by Chris Vuille, Vuille, Chris
Earth and Planetary Sciences · Mathematics · Physics and Astronomy · #Adiabatic process #Astrophysics #Constant (computer programming) #Cosmology and Gravitation Theories #Equation of state #Geophysics and Gravity Measurements #Mathematics #Neutrino #Neutron #Neutron star #Nuclear physics #Order (exchange) #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Stars #State (computer science) #Supernova #astro-ph
paper · pdf · doi:10.48550/arxiv.0812.3828
original figures and tables are no longer available
arxiv created 2008/12/19 · openalex publication_date 2008/12/19 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The equation of state for matter with energy density above 2 x1014 g/cm3 is parametrized by P = kNGamma, where N is the number density, Gamma is the adiabatic index, and k a constant. Using this scheme to generate thousands of models, together with data on neutron star masses, it is found, for a core region with a constant adiabatic index, that the central density must satisfy 1015 gm/cm3 < rhoc < 1016 gm/cm3, with Gamma > 2.2. Further preliminary results indicate, based on the observed neutrino flux from supernova 1987a, that this number must be considerably higher, on the order of 3.5. These results provide evidence for a hard equation of state in the cores of neutron stars.