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We describe two fitting schemes that aim to represent the high-density partof realistic equations of state for numerical simulations such as neutron staroscillations. The low-density part of the equation of state is represented byan arbitrary polytropic crust, and we propose a generic procedure to stitch anydesired crust to the high-density fit, which is performed on the internalenergy, pressure and sound speed of barotropic equations of state that describecold neutron stars in $\beta$-equilibrium. An extension of the fitting schemesto equations of state with an additional compositional parameter is proposed.In particular we develop a formalism that ensures the existence of a$\beta$-equilibrium at low densities. An additional feature of this low-densitymodel is that it can be, in principle, applied to any parametrization. Theperformance of the fits is checked on mass, radius and tidal deformability aswell as on the dynamical radial oscillation frequencies. To that end, we use apseudospectral isolated neutron star evolution code based on a non-conservativeform of the hydrodynamical equations. A comparison to existing parametrizationsis proposed, as far as possible, and to published radial frequency values inthe literature. The static and dynamic quantities are well reproduced by thefitting schemes. Our results suggest that, even though the radius is verysensitive to the choice of the crust, this choice has little influence on theoscillation frequencies of a neutron star.

One- and two-parameter equation of state parametrizations with continuous sound speed for neutron star simulations