  We review the state of the art regarding the computation of the resistance
coefficients in conditions typical of the stellar plasma, and compare the
various results studying their effect on the solar model. We introduce and
discuss for the first time in an astrophysical context the effect of quantum
corrections to the evaluation of the resistance coefficients, and provide
simple yet accurate fitting formulae for their computation. Although the
inclusion of quantum corrections only weakly modifies the solar model, their
effect is growing with density, and thus might be of relevance in case of
denser objects like, e.g., white dwarfs.
