Self-Consistent 3D Equations of State at Finite Temperatures for Supernovae and Neutron Stars.

Details Self-Consistent 3D Equations of State at Finite Temperatures for Supernovae and Neutron Stars. Self-Consistent 3D Equations of State at Finite Temperatures for Supernovae and Neutron Stars.

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...207.1707s&link_type=abstract

American Astronomical Society Meeting 207, #17.07; Bulletin of the American Astronomical Society, Vol. 37, p.1182

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We present the first results from a fully self-consistent, temperature-dependent equation of state that spans the whole density range of neutron stars and supernova cores. The equation of state is calculated using a mean-field Hartree-Fock method in three dimensions with no symmetry constraints. The nuclear interaction is represented by a phenomenological model such as the Skyrme or separable potential. The calculation scheme we employ naturally allows effects such as (i) neutron drip, which results in an external neutron gas, (ii) the variety of exotic nuclear shapes expected for extremely neutron heavy nuclei, and (iii) the subsequent dissolution of these nuclei into nuclear matter. In this way we are able to calculate the equation of state across phase transitions without recourse to interpolation techniques between density regimes described by different physical models. This work was performed under the auspices of the TeraScale Supernova Initiative, funded by SciDAC grants from the DOE Office of Science High-Energy, Nuclear, and Advanced Scientific Computing Research Programs.

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