南極天壇陣列辨別極高能宇宙微中子風味比靈敏度之模擬

Abstract

偵測極高能宇宙微中子是了解未知高能宇宙射線源的途徑之一，而其中微中子的風味比例除了帶有來自射線源物理特性的資訊，亦受到在傳播過程中微中子振盪和牽涉到的非標準物理的影響。一種相當具有前景的微中子偵測法是接收由微中子在密介質中反應後產生簇射所發出的無線電波段契忍可夫輻射。而不同風味的微中子與物質間載荷流交互作用所產生的帶電輕子在介質中有不同的能量損失特性，提供了我們分辨不同微中子風味的線索。在本文中，我們建構了模擬來得到南極天壇陣列(ARA)微中子事件的方向分布，並探討利用方向分布辨別微中子風味比的可行性。

Detecting Ultra-high energy (UHE) cosmic neutrino is one of the routes to determine and understand the yet unknown origin of ultra-high energy cosmic rays (UHECRs). In addition, the flavor composition of UHE cosmic neutrinos carries the information about physical properties of their sources as well as the neutrino oscillation and possible exotic physics involved in the propagation. One promising UHE neutrino detection method is observing coherent Cherenkov radiation in radio frequencies generated by the shower induced by neutrino-matter interaction in dense medium, based on the Askaryan effect. Since different leptons have different energy-loss behaviors in the medium, the lepton production of neutrino via charged-current (CC) interaction with matter gives us clues to discriminate among different flavors. In this thesis, we build a simulation to study the expected direction distribution of detected neutrino events for the recently under-constructed Askaryan Radio Array (ARA) observatory at the South Pole, and investigate its potentiality as a tool for flavor ratio identification.