M Baldoncini, V Strati, S A Wipperfurth, G Fiorentini, F Mantovani, W F McDonough, B Ricci
备注：
7 pages including 2 figures and 1 table, in XIV International Conference on Topics in Astroparticle and Underground Physics (TAUP 2015) IOP Publishing , published on Journal of Physics: Conference Series 718 (2016) 062003
In the heart of the Creighton Mine near Sudbury (Canada), the SNO+ detector is foreseen to observe almost in equal proportion electron antineutrinos produced by U and Th in the Earth and by nuclear reactors. SNO+ will be the first long baseline experiment to measure a reactor signal dominated by CANDU cores ($\sim$55\% of the total reactor signal), which generally burn natural uranium. Approximately 18\% of the total geoneutrino signal is generated by the U and Th present in the rocks of the Huronian Supergroup-Sudbury Basin: the 60\% uncertainty on the signal produced by this lithologic unit plays a crucial role on the discrimination power on the mantle signal as well as on the geoneutrino spectral shape reconstruction, which can in principle provide a direct measurement of the Th/U ratio in the Earth.
SNOLAB是世界上最深的地下实验室之一，覆盖层为2092米。SNO+探测器的设计是为了实现几个基本的物理目标，作为一个低背景实验，特别是测量地球的地中微子通量。在这里，我们评估的影响，2公里的覆盖层上预测的地壳地中微子信号在SNO+。探测器周围50 x 50 km上地壳的精细3D模型和完整的生存概率计算用于模拟U和Th地中微子信号。将此信号与通过将SNO+放置在海平面获得的信号进行比较，我们突出显示了$1.4^{+1.8}_{-0.9}$ TNU信号差异，对应于总地壳贡献的~5%。最后，估计了从海平面延伸到~300米的额外地壳的影响。
Abundances of uranium and thorium elements in Earth estimated by geoneutrino spectroscopy
原始同位素$^{238}\mathrm{U}$、$^{235}\mathrm{U}$、$^{232}\mathrm{Th}$和$^{40}\mathrm{K}$的衰变对地球历史上的地热收支有贡献。因此，这些同位素的丰度是重建现代地球模型的关键参数。由铀和钍的放射性衰变产生的地中微子已被Kamioka液体闪烁反中微子探测器（KamLAND）观测到。这些测量已经改善了超过18年的观测时间，并改善了探测器的背景水平，主要是通过一个8年的几乎没有rector的时期，现在允许光谱与地中微子。我们的结果产生的第一个约束铀和钍的热量贡献。在此，KamLAND的结果是一致的地球化学估计的基础上的元素丰度的南极陨石和地幔橄榄岩。高Q模型在99.76% C. L.处不受欢迎。在5.2 $σ$中排除了完全放射成因模型，假定地幔中的产热元素分布均匀。
Towards imaging Earth's large-scale structures by directional geoneutrino detection with Ocean Bottom Detector
Tohoku University（东北大学）；University of Hawai'i at Mānoa（夏威夷大学马诺阿分校）；Lawrence Livermore National Laboratory（劳伦斯利弗莫尔国家实验室）；University of Maryland, College Park（马里兰大学帕克分校）；High Energy Accelerator Research Organization (KEK)（高能加速器研究机构（KEK））
IPHC, Université de Strasbourg, CNRS/IN2P3（斯特拉斯堡大学）；Pakistan Institute of Nuclear Science and Technology（巴基斯坦核科学与技术研究所）；Sun Yat-Sen University（中山大学）；The University of Liverpool（利物浦大学）；INFN Catania and Dipartimento di Fisica e Astronomia dell Università di Catania（意大利国家核物理研究所卡塔尼亚分部及卡塔尼亚大学物理与天文系）；Joint Institute for Nuclear Research（联合核研究所）；INFN Sezione di Milano and Dipartimento di Fisica dell Università di Milano（意大利国家核物理研究所米兰分部及米兰大学物理系）；IJCLab, Université Paris-Saclay, CNRS/IN2P3（巴黎萨克雷大学）；Institute of Physics and EC PRISMA + , Johannes Gutenberg Universität Mainz（美因茨约翰内斯·古腾堡大学）；INFN Milano Bicocca and University of Milano Bicocca（意大利国家核物理研究所米拉比科卡分部及米拉比科卡大学）
