  We analyse the implications of superfluid turbulence for neutron star
physics. We begin by extending our previous results for the mutual friction
force for a straight vortex array to account for the self-induced flow which
arises when the vortices are curved. We then discuss Vinen's phenomenological
model for isotropic turbulence, and derive the associated (Gorter-Mellink) form
for the mutual friction. We compare this derivation to a more recent analysis
of Schwarz, which sheds light on various involved issues. Having discussed
isotropic turbulence, we argue that this case is unlikely to be relevant for
neutron stars. Instead we expect a rotating neutron star to exhibit polarised
turbulence, where relative flow drives the turbulence and rotation counteracts
it. Based on recent results for superfluid Helium, we construct a
phenomenological model that should have the key features of such a polarised
turbulent system.
