Stars as Laboratories for Fundamental Physics - MPP Theory Group

Solar Neutrinos 361
Table 10.5. Predicted absorption rate (in SNU) by 37 Cl for different solar
source reactions. BP92 give “theoretical 3σ” uncertainties.
Diffusion pp pep 7 Be 8 B 13 N 15 O Total
BP95 He, metals 0.0 0.2 1.2 7.2 0.1 0.4 9.3 +1.2
−1.4
BP92 He 0.0 0.2 1.2 6.2 0.1 0.3 8.0 ± 3.0
BP92 — 0.0 0.2 1.2 5.5 0.1 0.2 7.2 ± 2.7
TL93 — 0.0 0.2 1.1 4.6 0.1 0.2 6.4 ± 1.4
BP92 = Bahcall and Pinsonneault (1992).
BP95 = Bahcall and Pinsonneault (1995).
TL93 = Turck-Chièze and Lopes (1993).
Fig. 10.8. Solar neutrino flux at the Homestake experiment (ν 37 e Cl →
37 Ar e) for the past quarter century. The shaded band indicates the 1σ
uncertainty of the global best-fit average neutrino flux (Lande 1995).
counters must be subtracted, the counting rate attributed to solar neutrinos
in a given run is sometimes found to be formally negative. In
those cases, a zero counting rate is adopted. The distribution of counting
rates for 99 runs (18−117) is shown in Fig. 10.7. The global average
given in Eq. (10.12) is based on a maximum-likelihood analysis which
includes the background. It would not be correct to average the data
points with individual background subtractions to obtain a global average
signal.