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研究生:曾玠郡
研究生(外文):Jie-Jun Tseng
論文名稱:在地球和天文環境中之微中子相關碰撞過程
論文名稱(外文):Neutrino Related Processes in Terrestrial and Astrophysical Colliders
指導教授:林貴林
指導教授(外文):Guey-Lin Lin
學位類別:博士
校院名稱:國立交通大學
系所名稱:物理研究所
學門:自然科學學門
學類:物理學類
論文種類:學術論文
論文出版年:2002
畢業學年度:90
語文別:英文
中文關鍵詞:微中子
相關次數:
  • 被引用被引用:0
  • 點閱點閱:232
  • 評分評分:
  • 下載下載:44
  • 收藏至我的研究室書目清單書目收藏:0
在此篇論文之中, 我們深入地探討了“微子中”在各種不同的物理環境下所發生的有趣反應和現象, 其範圍涵蓋了離我們較近的地球表面, 和大氣層, 遠至我們身處的銀河系或距我們數千光年之遙的中子星和脈衝星。微中子本身就是個非常奇妙的基本粒子, 一直以來人們認為它是沒有質量的, 不過就在最近幾年的大氣層微中子和太陽微中子的量測實驗之中, 人們發現了微中子可以經由不同種類微中子之間的震盪來獲取質量的事實。不過它的質量還是非常的小, 小到還不及電子的千萬分之一。微中子另一個奇特的地方就是它那不太理會其它粒子的個性, 彷彿是個絕世的隱者, 從來不與外人打交道, 之所以這樣形容它是因為微中子向來只參與弱作用的反應, 而弱作用反應的強度卻是非常微小, 因而造就了它那特立獨行的性格。不過也正因為微中子的質量小所以它的速度快, 因為不太參與反應所以跑得遠, 又快又遠而讓我們可以藉由觀察它來認識離我們人類所無法到達的時空。在本篇的第一個部分, 我們估算了在強磁場下光子和微中子的散射截面, 並且運用此一結果來估算微中子在某些致密星中的能量損耗率。而在第二個部分中, 我們估算了來自大氣層和我們所屬銀河系的陶-微中子流量, 並且揭露了伴著微中子的震盪效應而來的修正和改變。在最後我們還探討了在一些興建中或是已經就緒的高能微中子望遠鏡實驗其所能觀測到的頻率和能量限制。在最後一個部分, 我們則探討了在 Zee模型的框架下有可能在地表上的對撞器之中所觀測到的現象, 例如中性希格斯粒子衰變到二個光子, 或是帶電希格斯粒子的衰變… 等等。 我們並且估算了中性希格斯粒子可能的質量範圍和一些相關耦合常數的大小。

\contentsline {chapter}{\numberline {1}Introduction}{1}
\contentsline {chapter}{\numberline {2}Neutrino-Photon Interactions in highly magnetized stars}{4}
\contentsline {section}{\numberline {2.1}The Effects of Magnetic Field}{4}
\contentsline {section}{\numberline {2.2}Fermion Propagator in a Background Magnetic Field}{6}
\contentsline {subsection}{\numberline {2.2.1}The Exact Solution for the Fermion Propagator}{6}
\contentsline {subsection}{\numberline {2.2.2}The Weak Field Limit}{10}
\contentsline {subsection}{\numberline {2.2.3}The Phase Factor}{17}
\contentsline {section}{\numberline {2.3}Neutrino-Photon Interactions}{19}
\contentsline {subsection}{\numberline {2.3.1}$\gamma \gamma \to \nu \mathaccent ? {\nu }$}{19}
\contentsline {subsection}{\numberline {2.3.2}$\gamma \to \nu \mathaccent ? {\nu }$ and $\nu \to \nu \gamma $}{23}
\contentsline {chapter}{\numberline {3}The Flux of High-Energy Atmospheric and Galactic Tau Neutrinos}{31}
\contentsline {section}{\numberline {3.1}The Production of High-Energy Tau Neutrinos}{31}
\contentsline {section}{\numberline {3.2}The Intrinsic Atmospheric Tau Neutrinos}{34}
\contentsline {subsection}{\numberline {3.2.1}The Cascade Equations for Atmospheric Tau Neutrinos}{34}
\contentsline {subsection}{\numberline {3.2.2}The Solutions for the Cascade Equations}{36}
\contentsline {subsection}{\numberline {3.2.3}The Results}{38}
\contentsline {section}{\numberline {3.3}The Intrinsic Galactic Tau Neutrinos}{39}
\contentsline {subsection}{\numberline {3.3.1}The Flux Formula in a Simplified Galaxy Model}{40}
\contentsline {subsection}{\numberline {3.3.2}Galactic Tau Neutrino Production}{41}
\contentsline {subsubsection}{Via $D_s$ mesons}{41}
\contentsline {subsubsection}{Via $b\mathaccent ? {b}$, $t\mathaccent ? {t}$, $W^*$ and $Z^*$}{44}
\contentsline {section}{\numberline {3.4}Effects of Neutrino Flavor Oscillations and Prospects for Observations}{45}
\contentsline {chapter}{\numberline {4}The Higgs Boson Phenomenology in the Neutrino Motivated Zee Model}{49}
\contentsline {section}{\numberline {4.1}The Zee Model}{50}
\contentsline {subsection}{\numberline {4.1.1}The Lagrangian of the Zee Model}{50}
\contentsline {subsection}{\numberline {4.1.2}The Higgs Potential}{51}
\contentsline {subsection}{\numberline {4.1.3}The Neutrino Masses}{53}
\contentsline {section}{\numberline {4.2}Constraints on the Higgs Sector Parameters through Renormalization Group Equations}{56}
\contentsline {subsection}{\numberline {4.2.1}The Renormalization Group Equations}{56}
\contentsline {subsection}{\numberline {4.2.2}The Constraints}{58}
\contentsline {subsection}{\numberline {4.2.3}The Numerical Results}{60}
\contentsline {section}{\numberline {4.3}The Higgs Boson Phenomenology in the Zee Model}{70}
\contentsline {subsection}{\numberline {4.3.1}Two-Photons Decay Width of the Lightest Neutral Higgs Boson}{70}
\contentsline {subsection}{\numberline {4.3.2}The Phenomenology of Charged Higgs Bosons}{77}
\contentsline {chapter}{\numberline {5}Conclusions}{85}
\contentsline {chapter}{\numberline {A}The $C_i$ Coefficients for the $\gamma \gamma \to \nu \mathaccent ? {\nu }$ Process}{90}
\contentsline {chapter}{\numberline {B}The Model for Atmospheric Density}{92}
\contentsline {chapter}{\numberline {C}The Perturbative QCD Formulae for Charm Quark and $\nu _{\tau }$ Productions}{93}
\contentsline {chapter}{\numberline {D}The QGSM Formulae for the $D_s$ Productions}{95}

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%
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%
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%
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%

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