  We present updated constraints on dark matter models with momentum-dependent
or velocity-dependent interactions with nuclei, based on direct detection and
solar physics. We improve our previous treatment of energy transport in the
solar interior by dark matter scattering, leading to significant changes in
fits to many observables. Based on solar physics alone, DM with a
spin-independent $q^{4}$ coupling provides the best fit to data, and a
statistically satisfactory solution to the solar abundance problem. Once direct
detection limits are accounted for however, the best solution is spin-dependent
$v^2$ scattering with a reference cross-section of 10$^{-35}$ cm$^2$ (at a
reference velocity of $v_0=220$ km s$^{-1}$), and a dark matter mass of about 5
GeV.
