Solar models with energy transport by weakly interacting particles

Details Solar models with energy transport by weakly interacting particles Solar models with energy transport by weakly interacting particles

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...306..703g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 306, July 15, 1986, p. 703-709.

Astronomy and Astrophysics

Astrophysics

82

Energy Transfer, Solar Neutrinos, Stellar Structure, Weak Interactions (Field Theory), Energy Distribution, Flux (Rate), Stellar Evolution, Stellar Models, Temperature Distribution

Scientific paper

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.

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