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[PENDING] Elementary excitations in homogeneous neutron star matter

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FIG. 1: (Color online) The proton fraction as a function of total baryon density in neutron star matter
FIG. 2: (Color online) The proton dispersion relation in the jelly model. The energy ω 0 e is the electron plasmon energy at zero momentum
FIG. 3: (Color online) The four branches of the electron-proton system interacting by coulomb force only, under neutron star matter conditions
TABLE II: Density and model dependence of the residual interaction elements (bulk=momentum-independent part), effective masses, Fermi velocities and level densities
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