Nuclear constraints on the EoS and rotating neutron stars

Abstract

In this contribution nuclear constraints on the equation of state for a neutron star are discussed. A combined fit to nuclear masses and charge radii leads to improved values for the symmetry energy and its derivative at nuclear saturation density, $S_{\mathrm{v}}=31$ MeV and $L=68\pm 8$ MeV. As an application the sensitivity of some properties of rotating supramassive neutron stars on the EoS is discussed.

Comments: 5 pages, 4 figures. Talk presented at the Conference "The Modern Physics of Compact Stars and Relativistic Gravity", September 2013, Yerevan, Armenia