What do we (not) know theoretically about solar neutrino fluxes?

Details What do we (not) know theoretically about solar neutrino fluxes? What do we (not) know theoretically about solar neutrino fluxes?

2004-02-04

arxiv.org/abs/astro-ph/0402114v2

Phys.Rev.Lett. 92 (2004) 121301

Astronomy and Astrophysics

Astrophysics

Published version: Experimental S17 (8B nus) changed from 20.7 to 20.6

Scientific paper

10.1103/PhysRevLett.92.121301

Solar model predictions of 8B and p-p neutrinos agree with the experimentally-determined fluxes (including oscillations): phi(pp)_{measured} = (1.02 +- 0.02 +- 0.01)phi(pp)_{theory}, and phi(8B)_{measured} =(0.88 +- .04 +- 0.23)phi(8B)_{theory}, 1 sigma experimental and theoretical uncertainties, respectively. We use improved input data for nuclear fusion reactions, the equation of state, and the chemical composition of the Sun. The solar composition is the dominant uncertainty in calculating the 8B and CNO neutrino fluxes; the cross section for the 3He(4He, gamma)7Be reaction is the largest uncertainty for the calculated 7Be neutrino flux.

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