First results from KamLAND: evidence for reactor antineutrino disappearance.

By KamLAND-Zen Collaboration. Physical Review Letters, 2002

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KamLAND has measured the flux of nu;(e)'s from distant nuclear reactors. We find fewer nu;(e) events than expected from standard assumptions about nu;(e) propagation at the 99.95% C.L. In a 162 ton.yr exposure the ratio of the observed inverse beta-decay events to the expected number without nu;(e) disappearance is 0.611+/-0.085(stat)+/-0.041(syst) for nu;(e) energies >3.4 MeV. In the context of two-flavor neutrino oscillations with CPT invariance, all solutions to the solar neutrino problem except for the "large mixing angle" region are excluded.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/124fb61d9542619ab24bedced80d58e77b4cfd0d

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Citations in the corpus

Constraints on sterile neutrinos as dark matter candidates from the diffuse X-ray background (2005, background): “There are separate measurements of neutrino oscillations in solar neutrinos (Ahmad et al. 2002), atmospheric neutrinos (Fukuda et al. 1998), and reactor neutrinos (Eguchi et al. 2003).”
Sterile neutrinos in cosmology (2017, methodology): “utrinos in charge-current interactions [7]. This avor conversion was conrmed in the KamLAND laboratory reactor neutrino experiment, which sees the same avor conversion but with reactor antineutrinos [40]. The Super-Kamiokande atmospheric neutrino experiment sees a zenith angle dependence of the atmo”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, neutral): “…solar neutrinos (Davis et al. 1968; Cleveland et al. 1998; Hampel et al. 1999; Abdurashitov et al. 1999; Fukuda et al. 2001b,a; Ahmad et al. 2002; Ahmed et al. 2004), reactor neutrinos (Eguchi et al. 2003; Araki et al. 2005), and accelerator beam neutrinos (Ahn et al. 2003; Michael et al. 2006).”
Where are we with light sterile neutrinos? (2019, background): “If we had not thought broadly about the source of the solar neutrino anomalies and how matter could effect flavor change – which led to the development of the MSW solution – we probably would have never proposed the KamLAND experiment [17], and would remain greatly confused about the three-neutrino ”
Dark energy from mass varying neutrinos (2003, neutral): “illations from the SuperKamiokande experiment [6], consistent with earlier evidence from the IMB experiment [7,8] and Kamiokande [9,10], and recently conﬁrmed by K2K [11–13]. The SNO [14] and KamLAND [15] experiments have conﬁrmed the neutrino oscillation interpretation of the solar neutrino deﬁcit ”
Series expansions for three-flavor neutrino oscillation probabilities in matter (2004, neutral): “The results of the atmospheric neutrino experiments [1, 2, 3] and the K2K accelerator neutrino experiment [4] have allowed the determination of the fundamental neutrino parameters ∆m(2)31 and θ23 to an accuracy of about 30% and 15%, respectively, while the solar neutrino experiments [5] and the KamL”
Shock Breakout in Core-Collapse Supernovae and Its Neutrino Signature (2002, background): “At resonance,θm = π/4 andLv/L0 = cos2θ, but for the range of densities that obtain in protoneutron stars and the values ofδm2 (∼ 5× 10−5eV2) and sin2 2θ (> 0.8) derived from the KamLAND (Eguchi et al. 2003) and solar neutrino data, there are no MSW resonances in supernova interiors.”