Abstract
Weakly interacting, massive particles (WIMPs) have recently been proposed as a solution to the solar neutrino problem1–3. Whereas standard solar models consistently predict a detection rate of (high-energy) neutrinos 3 times higher than that observed in the Davis experiment4–6, the presence of hypothetical massive particles in the solar centre would resolve this discrepancy. Models which incorporate a relative number of 10−11 WIMPs with appropriate scattering cross-section would reduce the predicted neutrino detections by 37Cl to the observed value, without significant changes in the solar structure outside the central region1–3. We have subjected these models to an observational test of p–mode oscillation frequencies by computing frequency differences of low-degree, high-order oscillation frequencies. Although standard solar models also pass this test, WIMP models provide a better fit.
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Däppen, W., Gilliland, R. & Christensen-Dalsgaard, J. Weakly interacting massive particles, solar neutrinos, and solar oscillations. Nature 321, 229–231 (1986). https://doi.org/10.1038/321229a0
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DOI: https://doi.org/10.1038/321229a0
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