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完整後設資料紀錄
DC 欄位 | 值 | 語言 |
---|---|---|
dc.contributor.advisor | 陳丕燊(Pisin Chen) | |
dc.contributor.author | Shi-Hao Wang | en |
dc.contributor.author | 王士豪 | zh_TW |
dc.date.accessioned | 2021-06-17T00:27:55Z | - |
dc.date.available | 2012-03-19 | |
dc.date.copyright | 2012-03-19 | |
dc.date.issued | 2012 | |
dc.date.submitted | 2012-02-14 | |
dc.identifier.citation | [1] W. Hanlon,http://www.physics.utah.edu/~whanlon/spectrum.html
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dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/66266 | - |
dc.description.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。 | zh_TW |
dc.description.abstract | 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. | en |
dc.description.provenance | Made available in DSpace on 2021-06-17T00:27:55Z (GMT). No. of bitstreams: 1 ntu-101-R98244005-1.pdf: 3744209 bytes, checksum: 0db04dfd4d86ac3995d28817a85086b9 (MD5) Previous issue date: 2012 | en |
dc.description.tableofcontents | Contents
1 Introduction 1 1.1 Mysteries of Cosmic Rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.1.1 Cosmic rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.1.2 How are cosmic rays accelerated? . . . . . . . . . . . . . . . . . . . . . . 2 1.1.3 Where do cosmic rays come from? . . . . . . . . . . . . . . . . . . . . . . 2 1.1.4 The GZK Process and the End of Cosmic Ray Spectrum . . . . . . . . . 4 1.2 Interconnection between UHE Cosmic Rays, Neutrinos, and Gamma Rays . . . . 6 1.3 Ultra-High Energy Cosmic Neutrinos . . . . . . . . . . . . . . . . . . . . . . . . 6 1.4 Ultra-High Energy Cosmic Neutrino Detection and Observatories . . . . . . . . 8 1.4.1 Basic Concepts . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 1.4.2 Askaryan Effect . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9 1.4.3 Optical Cherenkov Detection . . . . . . . . . . . . . . . . . . . . . . . . . 10 1.4.4 Extensive Air Shower Detection . . . . . . . . . . . . . . . . . . . . . . . 11 1.4.5 Radio Cherenkov Detection . . . . . . . . . . . . . . . . . . . . . . . . . 12 1.4.6 Acoustic Detection . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 16 2 Flavor Ratios of UHE Cosmic Neutrinos 17 2.1 Neutrino Oscillation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17 2.2 Understanding UHECR Source Properties from Neutrino Flavor Ratios . . . . . 19 2.3 Neutrino Flavor Ratio as a Probe of Non-Standard Physics . . . . . . . . . . . 19 2.4 Strategies for Measuring Flavor Ratios . . . . . . . . . . . . . . . . . . . . . . . 20 2.4.1 Event Topologies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 3 Simulation Setup 23 3.1 Overview . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23 3.2 Neutrino Generation and Propagation with MMC . . . . . . . . . . . . . . . . . 23 3.2.1 General Description of MMC . . . . . . . . . . . . . . . . . . . . . . . . 23 iii3.2.2 Generation and Selection of Neutrino Samples . . . . . . . . . . . . . . . 24 3.3 Neutrino Event Detection with SADE . . . . . . . . . . . . . . . . . . . . . . . 27 3.3.1 Detector Configuration . . . . . . . . . . . . . . . . . . . . . . . . . . . . 27 3.3.2 Ice Properties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 27 3.3.3 Shower Generation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 28 3.3.4 Ray Tracing . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 30 3.3.5 Generation and Propagation of Cherenkov Radiation . . . . . . . . . . . 31 3.3.6 Detector Response and Trigger Rules . . . . . . . . . . . . . . . . . . . . 32 4 Direction Distribution of Observed Neutrino Events 37 4.1 Statistics of Simulated Neutrino Events . . . . . . . . . . . . . . . . . . . . . . . 38 4.2 Cosmogenic Neutrino Flux and Flavor Ratios on the Earth . . . . . . . . . . . . 38 4.3 Interaction Probability . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 40 4.4 Detection Efficiency . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41 4.5 Event Direction Distribution and All-Sky Flavor Ratios of Events . . . . . . . . 43 5 Results 51 5.1 Reconstructing Neutrino Flavor Ratios from the Direction Distribution of De- tected Events . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 51 5.1.1 Preparing Pseudo-Data . . . . . . . . . . . . . . . . . . . . . . . . . . . 51 5.1.2 Fitting Pseudo-Data . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 52 5.1.3 Flavor Resolution versus Number of Observed Events and Angular Res- olution . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 53 5.2 Systematic Uncertainties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 56 5.2.1 Systematic Uncertainty from Neutrino Spectrum . . . . . . . . . . . . . . 56 5.2.2 Systematic Uncertainty from the Assumption of ν µ -ν τ Symmetry . . . . . 60 6 Conclusion and Future Works 65 A Calculation of Radiation Spectrum in SADE 73 B Uncertainty Estimation of Efficiency 77 | |
dc.language.iso | zh-TW | |
dc.title | 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 | zh_TW |
dc.title | Simulation of Askaryan Radio Array Neutrino Events for the Identification of Flavor Ratios | en |
dc.type | Thesis | |
dc.date.schoolyear | 100-1 | |
dc.description.degree | 碩士 | |
dc.contributor.oralexamcommittee | 林貴林(Guey-Lin Lin),黃美玲(Melin Huang),南智佑(Jiwoo Nam),劉宗哲(Tsung-Che Liu) | |
dc.subject.keyword | 極高能宇宙微中子,GZK微中子,微中子風味比,南極天壇陣列,事件方向分布, | zh_TW |
dc.subject.keyword | Ultra-high energy cosmic neutrino,cosmogenic (GZK) neutrino,neutrino flavor ratio,Askaryan Radio Array (ARA),direction distribution of events, | en |
dc.relation.page | 78 | |
dc.rights.note | 有償授權 | |
dc.date.accepted | 2012-02-14 | |
dc.contributor.author-college | 理學院 | zh_TW |
dc.contributor.author-dept | 天文物理研究所 | zh_TW |
顯示於系所單位: | 天文物理研究所 |
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