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

Understand

We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and $\beta$-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 $\Delta(1232)$ 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 $\beta$-stable nuclear matter to compute various structural properties of non-rotating neutron stars.The EOS is derived using the Brueckner--Bethe--Goldstone quantum many-body theory in the Brueckner--Hartree--Fock approximation.
• Neutron star properties are next computed solving numerically the Tolman--Oppenheimer--Volkov structure equations.