Measurement of the solar neutrino capture rate with gallium metal. III: Results for the 2002--2007 data-taking period

By S. C. J. N. Abdurashitov, V. Gavrin, V. Gorbachev, P. P. Gurkina, T. Ibragimova, A. Kalikhov, N. G. Khairnasov, T. Knodel, I. Mirmov, A. Shikhin and 9 more. 2009

530 citations recorded by the source corpus.

The Russian-American experiment SAGE began to measure the solar neutrino capture rate with a target of gallium metal in December 1989. Measurements have continued with only a few brief interruptions since that time. In this article we present the experimental improvements in SAGE since its last published data summary in December 2001. Assuming the solar neutrino production rate was constant during the period of data collection, combined analysis of 168 extractions through December 2007 gives a capture rate of solar neutrinos with energy more than 233 keV of $65.{4}_{\ensuremath{-}3.0}^{+3.1}$ (stat) ${}_{\ensuremath{-}2.8}^{+2.6}$ (syst) SNU. The weighted average of the results of all three Ga solar neutrino experiments, SAGE, Gallex, and GNO, is now $66.1\ifmmode\pm\else\textpm\fi{}3.1$ SNU, where statistical and systematic uncertainties have been combined in quadrature. During the recent period of data collection a new test of SAGE was made with a reactor-produced $^{37}\mathrm{Ar}$ neutrino source. The ratio of observed to calculated rates in this experiment, combined with the measured rates in the three prior $^{51}\mathrm{Cr}$ neutrino-source experiments with Ga, is $0.87\ifmmode\pm\else\textpm\fi{}0.05$. A probable explanation for this low result is that the cross section for neutrino capture by the two lowest-lying excited states in $^{71}\mathrm{Ge}$ has been overestimated. If we assume these cross sections are zero, then the standard solar model including neutrino oscillations predicts a total capture rate in Ga in the range of 63 SNU to 66 SNU with an uncertainty of about 4%, in good agreement with experiment. We derive the current value of the neutrino flux produced in the Sun by the proton-proton fusion reaction to be ${\ensuremath{\phi}}_{\mathit{pp}}^{\ensuremath{\bigodot}}=(6.0\ifmmode\pm\else\textpm\fi{}0.8)\ifmmode\times\else\texttimes\fi{}{10}^{10}/({\mathrm{cm}}^{2} \mathrm{s})$, which agrees well with the $\mathit{pp}$ flux predicted by the standard solar model. Finally, we make several tests and show that the data are consistent with the assumption that the solar neutrino production rate is constant in time.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f856eef338a873c8bedc87dfd2bf50216111fc5d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Nuclear and High Energy Physics

1. M. Drewes
2. Z. Xing
3. M. Tórtola
4. Julien Lesgourgues
5. M. Maltoni
6. S. Pastor
7. Y. Farzan
8. T. Schwetz

Citations in the corpus

• Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics (2020, methodology): “The complete data set used, as well as the parameters to which they are sensitive, are (1) from solar neutrino data [298, 413, 414, 415, 416, 417, 418, 419, 420, 421]: θ12, ∆m(2)21, and θ13; (2) from neutrino mode in long-baseline experiments K2K [422], MINOS [423, 424], T2K [425, 426], and NOνA [42”
• Solar Neutrinos: Status and Prospects (2012, methodology): “The weighted average (SAGE Collaboration, J. N. Abdurashitov et al. 2009) for the four calibrations, expressed as the ratio R of measured 71Ge to that expected due to the source strength, is R = 0.87 ± 0.05 (1σ).”
• Sterile Neutrino Fits to Short-Baseline Neutrino Oscillation Measurements (2012, methodology): “Indications of 𝜈 𝑒 disappearance have recently been published from calibration data taken by the SAGE [39] and GALLEX [40] experiments.”
• Neutrino Oscillations and Non-standard Interactions (2017, methodology): “Solar neutrino analysis include the historical radiochemical experiments Homestake [42], Gallex/GNO [43], SAGE [44], sensitive only to the interaction rate of electron neutrinos, but not to their energy or arrival time to the detector.”
• Three-flavour neutrino oscillation update (2008, result): “ recent discussion in [38]. Three-flavour neutrino oscillation update 10 SAGE: In our present analysis we have updated the capture rate of solar neutrinos measured in SAGE: 65.4+3 .1 −3.0 +26 −2.8 SNU [39], compared to the previous value 66.9 +3.9 −3.8 6 −3.2 SNU [40]. Note that the recently publishe”
• Updated fit to three neutrino mixing: status of leptonic CP violation (2014, methodology): “In the analysis of solar neutrino experiments we include the total rates from the ra- diochemical experiments Chlorine [19], Gallex/GNO [20] and SAGE [21].”
• Neutrino Mass Ordering from Oscillations and Beyond: 2018 Status and Future Prospects (2018, background): “…are rather well measured by the solar experiments (Cleveland et al., 1998; Hosaka et al., 2006; Aharmim et al., 2008, 2010; Cravens et al., 2008; Abdurashitov et al., 2009; Kaether et al., 2010; Abe et al., 2011b; Bellini et al., 2014; Nakano, 2016) and the long-baseline reactor experiment…”
• Where are we with light sterile neutrinos? (2019, methodology): “Deficits of νe interactions were observed – compared to prediction – in the SAGE [1] and Gallex [2] experiments, with a threshold of 0.23 MeV; the Homestake experiment [3], with a threshold of 0.8 MeV; and the Kamioka [4] and early-Super-K data sets [5], with a threshold of 7 MeV.”