Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days

Abstract

The first results of the solar neutrino flux measurement from Super-Kamiokande are presented. The results shown here are obtained from data taken between 31 May 1996, and 23 June 1997. Using our measurement of recoil electrons with energies above 6.5 MeV, we infer the total flux of 8 B solar neutrinos to be 2.42 6 0.06͑stat͒ 10.10 20.07 ͑syst͒ 3 10 6 cm 22 s 21 . This result is consistent with the Kamiokande measurement and is 36% of the flux predicted by the BP95 solar model. The flux is also measured in 1.5 month subsets and shown to be consistent with a constant rate. [S0031-9007(98)06804-5] PACS numbers: 26.65. + t, 95.85.Ry, 96.40.Tv

COLA with massive neutrinos

“…In this paper we demonstrate how to extend this method to incorporate both modified gravity and massive neutrinos simultaneously in a quasi-nonlinear manner. The method is quasi-nonlinear because we only consider a linear neutrino density perturbation, such that the total density matter perturbation is defined δ m = (ρ cb δ cb + ρ ν δ (1) ν )/ρ m where we track non-linearities only in δ cb . Here the subscripts 'm', 'cb', and 'ν' represent the total matter, cold dark matter + baryon, and massive neutrino components respectively.…”

“…Observations of neutrino flavour oscillations [1,2] demand that at least two of the neutrino states are massive [3]. While the absolute mass of each of the three mass eigenstates is unknown, there are strong constraints on the difference in mass between the states which implies that at least one of them has a mass greater than ∼0.06 eV.…”

Study of antineutrino oscillations using accelerator and atmospheric data in MINOS

“…The deficit of ν e s in the neutrino flux from the Sun in comparison to the SSM, which was observed in many experiments such as Homestake 5 , GALLEX 6 , GNO 7 , SAGE 8 , SNO 9 , Kamiokande and Super-Kamiokande (Super-K) [29][30][31][32][33][34][35], shown in Figure 1.4, is known as the solar neutrino anomaly. [36].…”

Measurement of inclusiveπ0production in the charged-current interactions of neutrinos in a 1.3-GeV wide band beam

“…After the observation of solar neutrino and atmospheric neutrino oscillations [1][2][3][4][5][6][7] and their confirmation respectively at reactors [8] and accelerators [9], the primary aim of current and future neutrino experiments is to measure the θ 13 mixing angle, and to improve accuracy in the measurement of oscillation parameters. One of the largest limitations of accelerator-based neutrino experiments comes from the poor experimental knowledge of neutrino cross sections in the GeV energy range.…”