  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, $S_{\rm{v}}= 31$ 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.
