[en] Transport properties of stellar matter are important ingredients in understanding stellar evolution and stellar structure. Using theoretical techniques that have proven useful in solid state physics, Fermi liquid theory, and the theory of liquid metals, we have calculated the electron contribution to the electrical conductivity, the thermal conductivity, and the viscosity of neutron star matter in the absence of magnetic fields for densities less than 2 x 10¹⁴ g cm^-3 (regions where there is solid matter). The results are also applicable to high-density white dwarf matter. Variational solutions of the transport equations are used except where exact solutions exist. Transport by electrons of any energy both in the presence of a lattice and without the lattice present are considered. At temperatures very much below the Debye temperature of the lattice we have been able to do only an approximate treatment of the electron-phonon interaction, and for temperatures above the melting temperatures of the lattice ionic correlations are included. Relativistic electron-electron scattering is considered, as is electron-impurity and electron-neutron scattering. This work complements previous investigations of transport properties and extends the density regions over which we know the transport properties of dense matter