Solar models with energy transport by weakly interacting particles

Accretion by the sun of weakly interacting massive particles (WIMPs or cosmions) from a background population leads to efficient nonlocal energy transport in the solar core. At concentrations as low as 10 to the -11th by number, such particles, with ideal scattering cross sections, can lower the central temperature sufficiently to bring the predicted neutrino detection rate into agreement with observations. Since the perturbation is restricted to a small core, only small adjustments to the free parameters (initial hydrogen abundance and convection mixing length) are required to produce standard solar models with significantly lower (high-energy) neutrino fluxes.