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Determination of Solar Neutrino Oscillation Parameters using 1496 Days of Super-Kamiokande-I Data
High Energy Physics - Experiment · Submitted 22 May 2002
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim A global fit combining SK data with the solar neutrino interaction rates measured by Homestake, SNO, Gallex/GNO and SAGE prefers a single allowed area, the Large Mixing Angle solution, at the 98.9% confidence level.
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The abstract, sentence by sentence
A number of different fits to solar neutrino mixing and mass square difference were performed using 1496 days of Super-Kamiokande-I's solar neutrino data. These data select two allowed areas at large neutrino mixing when combined with either the solar $^8$B flux prediction of the standard solar model or the SNO interaction rate measurements. A global fit combining SK data with the solar neutrino interaction rates measured by Homestake, SNO, Gallex/GNO and SAGE prefers a single allowed area, the Large Mixing Angle solution, at the 98.9% confidence level. The mass square difference $\Delta m^2$ between the two mass eigenstates ranges from about 3 to $19\times10^{-5}$eV$^2$, while the mixing angle $\theta$ is in the range of $\tan^2\theta\approx$0.25--0.65.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | A number of different fits to solar neutrino mixing and mass square difference were performed using 1496 days of Super-Kamiokande-I's solar neutrino data. | method 0.75 | 0.93 | 0.03 | asserted 0.98 |
| s1 | These data select two allowed areas at large neutrino mixing when combined with either the solar $^8$B flux prediction of the standard solar model or the SNO interaction rate measurements. | result 1.00 | 0.80 | 0.08 | asserted 0.98 |
| s2 | A global fit combining SK data with the solar neutrino interaction rates measured by Homestake, SNO, Gallex/GNO and SAGE prefers a single allowed area, the Large Mixing Angle solution, at the 98.9% confidence level. | result 1.00 | 0.85 | 0.82 | asserted 0.97 |
| s3 | The mass square difference $\Delta m^2$ between the two mass eigenstates ranges from about 3 to $19\times10^{-5}$eV$^2$, while the mixing angle $\theta$ is in the range of $\tan^2\theta\approx$0.25--0.65. | result 1.00 | 0.85 | 0.18 | asserted 0.97 |
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The paper
Original abstract
A number of different fits to solar neutrino mixing and mass square difference were performed using 1496 days of Super-Kamiokande-I's solar neutrino data. These data select two allowed areas at large neutrino mixing when combined with either the solar $^8$B flux prediction of the standard solar model or the SNO interaction rate measurements. A global fit combining SK data with the solar neutrino interaction rates measured by Homestake, SNO, Gallex/GNO and SAGE prefers a single allowed area, the Large Mixing Angle solution, at the 98.9% confidence level. The mass square difference $\Delta m^2$ between the two mass eigenstates ranges from about 3 to $19\times10^{-5}$eV$^2$, while the mixing angle $\theta$ is in the range of $\tan^2\theta\approx$0.25--0.65.
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References
How the literature uses it
58 arXiv papers cite this in 68 sentences
Papers whose main result relates to this one's
States the same result 3 papers
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Together with the rates of other experiments, the Super-Kamiokande results imply active solar neutrino oscillations and restrict neutrino mixing and mass square difference to lie within the LMA solution area.
Solar Neutrino Precision Measurements using all 1496 Days of Super-Kamiokande-I Data · 0.96
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From the combination of several experiments' results with those of Super-K, the Large Mixing Angle solution is uniquely allowed at the 98.1% confidence level; this global solar neutrino oscillation analysis is presented.
The recent results of solar neutrino measurements in Super-Kamiokande · 0.85
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We find that the Large Mixing Angle (LMA) solution is selected at the 99% C.L.; the best-fit parameters are \Delta m^2=5.6 \times 10^{-5} eV^2 and \theta=32^{\circ}.
Imprint of SNO neutral current data on the solar neutrino problem · 0.81
Papers citing it · 41 sentences without a confident label
Uses its data or values 5 papers
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[ref] and [ref] .
Improving LMA predictions with non standard interactions · $(ε_αβ^eP)_CC=(ε_αβ^eP)_NC =ε_αβ^eP$ · 0.91
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Neutrino's mass squared differences were determined from experiments [ref] of using neutrinos from the sun, accelerators, reactors, and atmosphere as [ref] , [equation] where $m_i (i=1-3)$ are mass values.
Matter-enhanced transition probabilities in quantum field theory · Introduction · 0.83
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[ref] and [ref] .
Improving LMA predictions with non-standard interactions: neutrino decay in solar matter? · $(ε_αβ^eP)_CC=(ε_αβ^eP)_NC =ε_αβ^eP$ · 0.93
Compares with it 1 paper
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The rates we obtained were confronted with the data from the Cl experiment [ref] , the Ga ones [ref] , the SuperKamiokande spectrum [ref] , the SNO rates and spectra [ref] , the Borexino spectra for $^8 B$ neutrinos [ref] and for the remaining fluxes [ref] [We recall that, as mentioned in the introduction, we neglect any possible time variation in the Ga rate and perform fits to its average value, see ref.
Light sterile neutrinos, spin flavour precession and the solar neutrino experiments · Field profiles and rates · 0.88
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Since the establishment of the neutrino flavour oscillations [ref] , the effect was consistently probed by several experiments [ref] .
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Particle physics has seen two historic discoveries in less than twenty years: the confirmation of the mechanism of electroweak symmetry breaking [ref] and the discovery of neutrino oscillations [ref] , both deservedly honored with the Nobel prize.
Neutrino oscillations and the seesaw origin of neutrino mass · Introduction · 0.97
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In the past decade, atmospheric [ref] , solar [ref] , reactor [ref] and long-baseline accelerator [ref] neutrino experiments have provided compelling evidence for the phenomenon of neutrino oscillations.
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