Non-Markovian effects in the solar neutrino problem

G. Gervino; G. Kaniadakis; A. Lavagno; M. Lissia; P. Quarati

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Non-Markovian effects in the solar neutrino problem

G. Gervino·G. Kaniadakis·A. Lavagno·M. Lissia·P. Quarati

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Abstract

The solar core, because of its density and temperature, is not a weakly-interacting or a high-temperature plasma. Collective effects have time scales comparable to the average time between collisions, and the microfield distribution influences the particle dynamics. In this conditions ion and electron diffusion is a non-Markovian process, memory effects are present and the equilibrium statistical distribution function differs from the Maxwellian one. We show that, even if the deviations from the standard velocity distribution that are compatible with our present knowledge of the solar interior are small, they are sufficient to sensibly modify the sub-barrier nuclear reaction rates. The consequent changes of the neutrino fluxes are comparable to the flux deficits that constitute the solar neutrino problem.

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G. Gervino, G. Kaniadakis, A. Lavagno, M. Lissia, P. Quarati. 1998-09-01. Non-Markovian effects in the solar neutrino problem. https://arxiv.org/abs/physics/9809001

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