发表机构
NASA/Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文综述空间基宇宙中微子探测技术，以地球为靶体，利用大气簇射产生光学和射电信号，并讨论现有实验限制及下一代实验设计。
AI 中文摘要
空间基中微子探测利用天体（地球、月球和太阳）作为中微子靶体和粒子级联产生器。这些级联（即簇射）含有大量带电粒子，主要是电子和正电子，它们可以形成可由轨道或气球载（针对地球）实验探测到的信号。本文重点讨论以地球作为中微子靶体，利用大气从广延大气簇射（EAS）中产生光学和射电信号。地球本身内部的级联也能在冰中产生阿斯卡良辐射，由于冰的射电透明性，冰内中微子诱导簇射的信号最终能折射出地球表面。这些不同技术对中微子味探测灵敏度和占空比（即实验有效运行时间比例）也有不同要求。例如，光学测量需在天文黑夜附近进行，且受月光水平和EAS观测方向云层分布的影响。射电技术可在近100%效率下运行，只要人为及其他背景源最小化。鉴于从亚轨道或低地球轨道（LEO）高度观测中微子诱导信号的距离，目前探测的中微子能量阈值对光学切伦科夫探测约为1 PeV以上，对射电探测为100 PeV以上。本章将详细阐述宇宙中微子相互作用的性质、簇射发展、光学和射电信号的产生与探测，并通过讨论利用这些信号对甚高能和超高能宇宙中微子通量设定限制的实验来实现。我们还将讨论下一代空间基宇宙中微子探测实验的设计和模拟性能。
英文摘要
Space-based neutrino detection employs celestial bodies, the Earth, moon, and the sun, as neutrino targets and particle cascade generators. These cascades, or showers, have an immense content of charged particles, mainly electrons and positrons, that can form signals that can be detected by orbiting or balloon-borne (for the Earth) experiments. Here the focus will be on the using the Earth as the neutrino target and using the atmosphere to generate optical and radio signals from extensive air showers (EAS). Cascades in the Earth itself can also generate Askaryan radiation in ice, where the radio transparency allows the signal from in ice neutrino-induced showers to eventually refract out of the Earth's surface. These different techniques also have different neutrino-flavor detection sensitivities and duty cycles, i.e. experimental live time fractions. For example, optical measurements need to be performed close to astronomical night and are also affected by the level of moonlight and distribution of clouds in the the viewing direction of the EAS. The radio technique can be operate with nearly 100\% efficiency, as long as sources of anthropogenic and other backgrounds are minimal. Given the distances for viewing the neutrino-induced signals from sub-orbital or low Earth orbit (LEO) altitudes, the neutrino energy thresholds for detection are currently above $\sim$ 1 PeV for optical Cherenkov detection and 100 PeV for radio detection. In this chapter, the nature of the cosmic neutrino interactions, shower development, and optical and radio signal generation and detection will be detailed. This will be done by discussing experiments that have used such signals to set limits on the very-high and ultra-high energy cosmic neutrino flux. We will also discuss the design and simulated performance of the next generation of space-based cosmic neutrino detection experiments.
CommentsPublished in The Encyclopedia of Cosmology. Set 2: Frontiers in Cosmology. Volume 2: Neutrino Physics and Astrophysics. Edited by Floyd W. Stecker. Published by World Scientific Publishing Co. Pte. Ltd., 2024. ISBN #9781800614512, pp. 303-365, Chapter 7
Journal refThe Encyclopedia of Cosmology. Set 2: Frontiers in Cosmology. Volume 2: Neutrino Physics and Astrophysics. Edited by Floyd W. Stecker. Published by World Scientific Publishing Co. Pte. Ltd., 2024. ISBN #9781800614512, pp. 303-365
DOI：10.1142/9789811282645_0007
