We calculate static properties of non-rotating neutron stars (NS's) using a microscopic
equation of state (EOS) for asymmetric nuclear matter, derived from the Brueckner-Bethe …

We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the
core based on modern microscopic calculations using the Argonne v 18 potential plus three …

We calculate the nucleonic equation of state within the Brueckner-Bethe-Goldstone
formalism using the Argonne υ 18 two-body interaction and a three-body interaction. We …

The equation of state (EoS) of hot and dense matter is a fundamental input to describe static
and dynamical properties of neutron stars, core-collapse supernovae and binary compact …

We study the properties of nonrotating and rotating neutron stars for a new set of equations
of state (EOSs) with different high-density behavior obtained using the extended field …

Context. An equation of state (EoS) of dense nuclear matter is a prerequisite for studies of
the structure and evolution of compact stars. A unified EoS should describe the crust and the …

We review the current status and recent progress of microscopic many-body approaches
and phenomenological models, which are employed to construct the equation of state of …

We present results for neutron star models constructed with a new equation of state for
nuclear matter at zero temperature. The ground state is computed using the auxiliary field …

We provide convenient parametrizations of the high-density nuclear equation of state
obtained within the Brueckner-Hartree-Fock approach using different modern nucleon …

The properties and structure of neutron stars are determined by the equation of state (EOS)
of neutron-rich stellar matter. While the collective flow and particle production in relativistic …