The Ground State of Matter at High Densities: Equation of State and Stellar Models

TLDR

We have content for each. Background: first line: "The equation of state of zero-temperature matter in complete nuclear equilibrium is given for mass densities below 5 X 10^14 g." That is background context. Purpose: from [Purpose, Mechanism] line: "We redetermine, taking into account the effect of the Coulomb lattice and using more recent nuclear mass extrapolations, the sequence of equilibrium nuclides present at mass densities between 10^? and 4.3 X 10^11 g, the point of neutron drip; and calculate the equation of state here." So purpose: to redetermine equilibrium nuclides sequence and calculate EOS. Mechanism: multiple lines: [Mechanism] lines: first: "For densities between 4.3 X 10^11 and 5 X 10^14 g the equation of state is taken from the calculations of Baym, Bethe, and Pethick; included is an extension of the equation of state to still higher densities, taken from the calculations of Pandharipande, which include the effects of hyperons." Also: "We calculate zero-temperature white-dwarf and neutron-star models for the equation of state." Also: "Moments of inertia, surface deformations, and mass quadrupole moments are calculated for slowly rotating neutron stars." So mechanism: use existing EOS calculations, extend to higher densities, compute white dwarf and neutron star models, calculate moments etc.

Abstract

view Abstract Citations (1426) References (17) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS The Ground State of Matter at High Densities: Equation of State and Stellar Models Baym, Gordon ; Pethick, Christopher ; Sutherland, Peter Abstract The equation of state of zero-temperature matter in complete nuclear equilibrium is given for mass densities below 5 X 1014 g . We redetermine, taking into account the effect of the Coulomb lattice and using more recent nuclear mass extrapolations, the sequence of equilibrium nuclides present at mass densities betv en 10' and 4.3 X 1011 g , the point of neutron drip; and calculate the equation of state here. For densities between 4.3 X 1011 and 5 X 1014 g the equation of state is taken from the calculations of Baym, Bethe, and Pethick; included is an extension of the equation of state to still higher densities, taken from the calculations of Pandharipande, which include the effects of hyperons. We calculate zero-temperature white-dwarf and neutron-star models for the equation of state. The maximum stable white-dwarf mass, the Chandrasekhar limit, is 1.00 io. The lightest stable neutron star has a mass 0.0925 M0 and a central density 1.55 X 1014 g cm-3 neutron stars between 0.0925 and 0.11 M0 are entirely solid. Moments of inertia, surface deformations, and mass quadrupole moments are calculated for slowly rotating neutron stars. Publication: The Astrophysical Journal Pub Date: December 1971 DOI: 10.1086/151216 Bibcode: 1971ApJ...170..299B full text sources ADS |