Equation of state of dense nuclear matter and neutron star structure from nuclear chiral interactions

Author： Bombaci Ignazio Logoteta Domenico

E-ISSN： 1432-0746|609|issue|A128-A128

ISSN： 0004-6361

Source： Astronomy & Astrophysics, Vol.609, Iss.issue, 2018-02, pp. : A128-A128

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Abstract

Aims. We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and β-stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the Δ(1232) isobar intermediate state. This EOS is provided in tabular form and in parametrized form ready for use in numerical general relativity simulations of binary neutron star merging. Here we use our new EOS for β-stable nuclear matter to compute various structural properties of non-rotating neutron stars.