臺灣博碩士論文加值系統

微中子的質量很輕，所以受到重力的影響很小。它不帶電荷所以不受電磁力的干擾，幾乎只有弱作用能改變其路徑，因此對於天文學這種研究長時間、大尺度的學問來說，微中子是很好的觀測工具。在這篇論文之中，我們探討τ微中子天文學的一些課題。在本論文的第一個部分，我們提出了一種半解析的方法，來計算由入射進地球的宇宙高能微中子與地球物質作用之後所產生且射出地球表面的τ輕子流。這些入射進地球的宇宙高能微中子的能量範圍在10^5 GeV至10^10 GeV之間。接著，我們就可計算出這些淺穿地球的τ輕子流能量光譜，並且將不同的宇宙微中子源 (AGN、GRB、GZK) 代入計算的結果來作分析比較。在本論文的第二個部分，我們指出了能量範圍在1 GeV至10^4 GeV 的τ微中子天文學的可能性。在這個能量範圍內，由於不同種類的大氣層背景微中子流數量上的差異，使我們在較低能量就能觀測到宇宙τ微中子，而宇宙μ微中子在較高能量才能觀測到。這裡我們主要討論在銀河平面產生的宇宙微中子。我們發現能量在10 GeV 以上時，銀河平面τ微中子的數量會超過大氣層τ微中子的數量。 因此，理論上來說，我們可以藉由偵測能量在10 GeV 以上的τ微中子來觀測銀河平面。然而，另一方面，能量在 10^6 GeV 以上的銀河平面μ微中子才有足夠多的數量超過大氣層μ微中子而讓我們藉由偵測它們來觀測銀河平面。

1.Introduction 1

2.Earth-skimming Tau Neutrinos and The nduced
Tau-Lepton Spectrum 4
2.1 Tau-Lepton Energy Spectrum 4
2.2 W Resonamce Contributions 8
2.3 The Results 10
2.4 Prospects of possible observations 17

3.Tau Neutrino Astronomy in GeV Energies 19
3.1 Galactic-Plane Neutrino Flux 20
3.2 The Intrinsic Atmospheric Neutrino Fluxes 22
3.2.1 Intrinsic Atmospheric Muon Neutrino 22
Flux
3.2.2 Intrinsic Atmospheric Tau Neutrino 29
Flux
3.3 The Atmospheric Tau Neutrino Flux With
Oscillations In the Two-Flavor Mixing
Sheme 34
3.3.1 The Downmard and Horizontal
Atmospheric Tau Neutrino Fluxes 34
3.3.2 The Upward Atmospheric Tau Neutri
no Flux 43
3.3.3 Comparison and Discussion 45
3.4 The Atmospheric Tau Neutrino Flux With
Oscillations In the Three-Flavor Mixing
scheme 50

4. conclusion 55

Appendix.A The iteration method for obtaining the
Z(E,X) and the F(E,X) 58

Appendix.B The neutrino oscillation probabilities
in the three-flavor mixing scheme 60

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