The main goal of the KamLAND reactor electron anti-neutrino experiment is a search for electron anti- neutrino oscillation using inverse- beta decay reaction in 1,000 ton of ultra-pure liquid scintillator. The data-set is 1490.8 days from Mar. 2002 to May 2007. The best-fit oscillation parameters are Delta m^{2}_{21} = 7.58^{+0.14}_{-0.13} (stat.) +/- 0.15 (syst.) x 10$^{-5} eV^{2} and tan^{2} theta_{12} = 0.56^{+0.10}_{-0.07} (stat.) ^{+0.10}_{-0.06} (syst.). The statistical significance for reactor electron anti-neutrino disappearance is 8.8 sigma, and an undistorted electron anti-neutrino energy spectrum is disfavored at > 5 sigma.
英文摘要：
The main goal of the KamLAND reactor electron anti-neutrino experiment is a search for electron anti-neutrino oscillation using inverse-beta decay reaction in 1,000 ton of ultra-pure liquid scintillator. The data-set is 1490.8 days from Mar. 2002 to May 2007. The best-fit oscillation parameters are Delta m^{2}_{21} = 7.58^{+0.14}_{-0.13} (stat.) +/- 0.15 (syst.) x 10$^{-5} eV^{2} and tan^{2}theta_{12} = 0.56^{+0.10}_{-0.07} (stat.) ^{+0.10}_{-0.06} (syst.). The statistical significance for reactor electron anti-neutrino disappearance is 8.8 sigma, and an undistorted electron anti-neutrino energy spectrum is disfavored at > 5 sigma.
Kamioka液体闪烁体反中微子探测器（KamLAND）首次在99.95%C. L.处探测到来自地球源的电子反中微子消失。用中微子振荡解释，与卡姆兰德数据的最佳拟合给出了混合角为1.0，质量平方差为6.9 x 10^-5 eV ^2，与太阳中微子问题的大混合角解非常吻合。假设CPT不变性，这个结果排除了太阳中微子问题在> 99.95%C. L的其他解。
Search for Diffuse Supernova Neutrino Background in the Full KamLAND Dataset with Neural-Network-Based Event Classification
Research Center for Neutrino Science, Tohoku University（东北大学中微子科学研究中心）；Department of Human Science, Obihiro University of Agriculture and Veterinary Medicine（带广畜产大学人类科学学院）
Observables sensitive to absolute neutrino masses. II
在Phys. Rev. D 75，053001（2007）[arXiv：hep-ph/0608060]的后续文章中，我们根据最近的中微子振荡数据（KamLAND、SNO和MINOS）和宇宙学观测（WMAP 5年和其他数据），报告了中微子质量混合参数的最新约束。我们讨论了它们的相互作用与最终的0 nu 2beta衰变结果在76-锗声称的海德堡-莫斯科合作的一部分，使用最近的评估相应的核矩阵元素，和他们的不确定性。我们还评论了Cuoricino最近设定的130-Te中的0 nu 2beta极限，以及KATRIN实验的预期极限或信号。
Comment on "Observation of electron-antineutrino disappearance at Daya Bay"
在最近的Letter by An et al. [arXiv：1203.1669]中，报道了在大亚湾进行的中微子混合角θ_{13}的非零值测量，其显著性为5.2个标准偏差。利用考虑系统误差相关性的拉力项构造的χ^2来确定sin^2 θ_{13}的值。本文指出，在非零核反应堆χ^2 -假设的框架下，将KamLAND混合参数直接应用于大亚湾核燃烧过程的非平衡地中微子谱实验，将产生很高的不确定度，从而使中微子混合角θ_{13}的实际值产生很大的失真。
Constraint on the solar $Δm^2$ using 4,000 days of short baseline reactor neutrino data
在KamLAND和SNO/Super-KamioKANDE之间的太阳$Δm^2$的测量中，存在一个众所周知的2 $σ$张力。太阳$Δm^2$的精确测定对于当前和未来的长基线CP破坏测量尤其重要。参考文献\cite{Seo:2018rrb}指出，目前正在进行的短基线反应堆中微子实验，大亚湾和RENO，也可以限制太阳$Δm^2$值，这一点在有限的系统不确定性考虑下通过GLoBES模拟得到了证明。在这项工作中，公开可用的数据，从大亚湾（1,958天）和RENO（2,200天）被用来约束太阳$Δm^2$。通过$Δm^2_{ee}$和$\sin^2 θ_{13}$测量验证我们的方法的讨论见附录A。利用该方法，分别和结合大亚湾和RENO资料，得到了太阳$Δm^2$的合理约束条件。我们发现大亚湾和RENO的组合数据在95% C. L.处设定了太阳$Δm^2$的上限为18 $\times 10^{-5}$ eV $^2$，包括系统和统计不确定性。该约束略高于KamLAND值的两倍。由于这一综合结果仍然是统计有限的，即使是由大亚湾数据驱动，限制将改善与此实验的额外运行。
An estimate of theta_14 independent of the reactor antineutrino flux determinations
在以前的论文[Phys. Rev. D 83，113013（2011）]中，我们已经表明太阳扇区数据（太阳和KamLAND）对参数θ_14敏感，编码电子中微子与第四个（基本上）无菌质量本征态的混合物。在这项工作中，我们证明，这样的数据更喜欢一个非零值的θ_14，这种偏好是完全退化的非零θ_13。在这份报告中，我们展示了最近从全球中微子数据分析中出现的θ_13> 0的证据，如何解除这种简并不利于无菌中微子混合的情况。通过从我们的分析中排除来自反应堆实验的总速率信息，我们将我们的结果与对它们的通量归一化的任何假设解开。通过这种方式，我们确定了在90% C. L.时sin ^2（θ_14）< 0.04的稳健上限。
Low Energy Threshold Analysis of the Phase I and Phase II Data Sets of the Sudbury Neutrino Observatory
Results are reported from a joint analysis of Phase I and Phase II data from the Sudbury Neutrino Observatory. The effective electron kinetic energy threshold used is T_eff=3.5 MeV, the lowest analysis threshold yet achieved with water Cherenkov detector data. In units of 10^6 cm^{-2} s^{-1}, the total flux of active-flavor neutrinos from 8B decay in the Sun measured using the neutral current (NC) reaction of neutrinos on deuterons, with no constraint on the 8B neutrino energy spectrum, is found to be Phi_NC = 5.140 ^{+0.160}_{-0.158} (stat) ^{+0.132}_{-0.117} (syst). These uncertainties are m…
Combined Analysis of all Three Phases of Solar Neutrino Data from the Sudbury Neutrino Observatory
We report results from a combined analysis of solar neutrino data from all phases of the Sudbury Neutrino Observatory. By exploiting particle identification information obtained from the proportional counters installed during the third phase, this analysis improved background rejection in that phase of the experiment. The combined analysis resulted in a total flux of active neutrino flavors from 8B decays in the Sun of (5.25 \pm 0.16(stat.)+0.11-0.13(syst.)) \times 10^6 cm^{-2}s^{-1}. A two-flavor neutrino oscillation analysis yielded \Deltam^2_{21} = (5.6^{+1.9}_{-1.4}) \times 10^{-5} eV^2 an…
