Nuclear constraints on the equation of state and rotating neutron stars

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, Sv = 31 MeV and L = 68 ± 8 MeV. As an application the sensitivity of some properties of rotating supramassive neutron stars on the EoS is discussed.