Abundance distribution of heavy nuclides up to a subnuclear density and the equation of state for gravitationally collapsing stars

Details Abundance distribution of heavy nuclides up to a subnuclear density and the equation of state for gravitationally collapsing stars Abundance distribution of heavy nuclides up to a subnuclear density and the equation of state for gravitationally collapsing stars

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..85..243o&link_type=abstract

Astrophysics and Space Science, vol. 85, no. 1-2, July 1982, p. 243-262.

Astronomy and Astrophysics

Astrophysics

Abundance, Equations Of State, Gravitational Collapse, Heavy Elements, Nuclides, Stellar Mass, Astrophysics, Baryons, Density Distribution, Neutrons, Particle Mass, Pressure Distribution

Scientific paper

With the use of the empirical equations for the binding and internal energies of heavy nuclides with density dependence, the abundance distribution of neutron-excess nuclides which appear up to some subnuclear density along the collapsing trajectory of a stellar core is calculated with an assumption of the beta-equilibrium condition. Using the abundance distribution thus derived, the quantities affecting the hydrodynamics of the core, such as the average mass number and the mass fraction of heavy nuclides, the mass fraction of free neutrons, the number of electrons per baryon, the average excitation energy per nucleus, and the entropy, the pressure and the adiabatic index of the system are then calculated. It is found that it is possible to obtain fairly reliable values of these physical quantities by introducing only the magic and near-magic number nuclides in the calculation, and that the results are hardly affected by the difference of the semi-empirical nuclear mass formula used to derive the binding energies of unknown nuclides and the formula of the grand partition function of these nuclides.

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