Oscillations in solar models with weakly interacting massive particles

Details Oscillations in solar models with weakly interacting massive particles Oscillations in solar models with weakly interacting massive particles

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324.1153g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 15, 1988, p. 1153-1157.

Astronomy and Astrophysics

Astrophysics

10

Particle Interactions, Solar Neutrinos, Solar Oscillations, Stellar Models, Weak Interactions (Field Theory), Particle Flux Density, Stellar Cores, Stellar Interiors, Vibration Mode

Scientific paper

Solar models containing concentrations as low as 10-11 by number of weakly interacting massive particles (WIMPs), accreted from a galactic background population, are consistent with the observed flux of high-energy solar neutrinos. The structural changes produced in the solar core have also been shown to produce changes in the oscillation frequencies of g-modes and p-modes of low angular degree and high radial order. In this paper the authors examine the predictions for solar oscillations over a large range of possible WIMP properties.

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