Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21723404l&link_type=abstract
American Astronomical Society, AAS Meeting #217, #234.04; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We extended the truncated Finite Range Thomas Fermi model (FRTF hereafter).
Adding an additional density-dependent interaction, we could adjust the nuclear incompressibiliy from 316MeV to 235MeV and also fit the properties of pure neutron matter near the saturation density. The new interaction is used to compute semi-infinite surface properties as well as properties of finite nuclei including the neutron skin thickness.
Compared to the truncated model, we obtain a lower critical temperature for bulk matter coexistence as well as a lower maximum neutron star mass.
Using the Wigner-Seitz approximation as in the truncated model, we construct the equation of state of hot dense matter. The spherical Wigner-Seitz approximation is extended to ellipsoidal, cylindrical and planar geometries to model deformed nuclei and pasta phases at subnuclear densities.
We compare the composition of the neutron star crust to previously published results.
Lattimer James M.
Lim Yeunhwan
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