Abstract
Dense matter found in compact objects, specifically neutron stars and supernovae, is very neutron rich. Therefore, a correct description of the symmetry-energy contribution to the nuclear energy is of great importance. We have studied the constraints on the symmetry energy obtained from nuclear mass measurements as well as neutron-star observations. For this purpose, we have used a set of unified equations of state of cold dense matter, based on generalised Skyrme energy-density functionals recently developed by the Brussels-Montreal collaboration. Both nuclear mass measurements and neutron-star observations suggest that an optimum value of the symmetry energy coefficient J is around 30 MeV. Moreover, comparing our EoSs with astrophysical observations favours a value of the slope of the symmetry energy L around 37 MeV.