The ANITA collaboration have reported observation of two anomalous events that appear to be $\varepsilon_{\rm cr} \approx 0.6$ EeV cosmic ray showers emerging from the Earth with exit angles of $27^\circ$ and $35^\circ$, respectively. While EeV-scale upgoing showers have been anticipated as a result of astrophysical tau neutrinos converting to tau leptons during Earth passage, the observed exit angles are much steeper than expected in Standard Model (SM) scenarios. Indeed, under conservative extrapolations of the SM interactions, there is no particle that can propagate through the Earth with probability $p > 10^{-6}$ at these energies and exit angles. We explore here whether "beyond the Standard Model" (BSM) particles are required to explain the ANITA events, if correctly interpreted, and conclude that they are. Seeking confirmation or refutation of the physical phenomenon of sub-EeV Earth-emergent cosmic rays in data from other facilities, we find support for the reality of the ANITA events, and three candidate analog events, among the Extremely High Energy Northern Track neutrinos of the IceCube Neutrino Observatory. Properties of the implied BSM particle are anticipated, at least in part, by those predicted for the "stau" slepton ($\tildeτ_R$) in some supersymmetric models of the fundamental interactions, wherein the stau manifests as the next-to-lowest mass supersymmetric partner particle.
ICECUBE对高能宇宙中微子的观测开创了超越标准模型探索宇宙和新物理的新纪元。在标准图中，虽然大部分$ν_μ$和$ν_e$是在源中产生的，但振荡将产生$ν_τ$ { \it en route}。某些超越SM的场景，比如与超轻型DM的交互，可以改变这种情况。因此，宇宙中微子流的味道成分可以打开探索某些超出SM场景的可能性，否则是无法进入的。我们表明，$τ$味在中微子味中占有特殊的地位，在阐明新的物理。将ANITA观察到的两个异常事件解释为$ν_τ$事件，使得tau的味道更加有趣。我们研究了如何检测的两个tau事件的ICECUBE约束的中微子与超轻暗物质的相互作用，并讨论了这种相互作用的影响，甚至更高的能量宇宙中微子可探测的未来射电望远镜，如ARA，ARIANNA和GRAND。我们还重新审视了$3+1$中微子计划作为一个解决方案的两个异常ANITA事件，并澄清了一个误解，存在于文献中的高能中微子在物质中的演化的$3+1$计划与散射的可能性核。我们表明，现有的界限上的磁通量的$ν_τ$与EeV的能量排除了这种解决方案的ANITA事件。我们表明，$3+1$解决方案可以保存从这个约束和约束的额外的相对论自由度在早期宇宙中打开的中微子与超轻暗物质的相互作用。
Seafloor Topography Enhances KM3NeT Sensitivity to ANITA-like Events
Harvard University（哈佛大学）；University of Wisconsin（威斯康星大学）；Universitat de Barcelona (UB)（巴塞罗那大学）；Emmanuel College, University of Cambridge（剑桥大学伊曼纽尔学院）；Instituto de Física Corpuscular (CSIC-Universitat de València)（粒子物理研究所（西班牙国家科学研究委员会-瓦伦西亚大学））
Generation of TeV Photons by PeV Neutrinos in Dense Astrophysical Environments
The Hong Kong University of Science and Technology（香港科技大学）；Jockey Club Institute for Advanced Study, The Hong Kong University of Science and Technology（香港科技大学聚龙高等研究院）；School of Physics, Peking University（北京大学物理学院）；Center for Gravitational Wave Experiment, National Microgravity Laboratory, Institute of Mechanics, Chinese Academy of Sciences（中国科学院力学研究所微重力国家实验室引力波实验中心）；Department of Physics, Chongqing University（重庆大学物理学院）；School of Physics, Zhengzhou University（郑州大学物理学院）
