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研究生: 李建和
論文名稱: 低質量原恆星源IRAS 16293-2422的分子清單
Molecular Inventory in the Low-mass Protostellar Source IRAS 16293-2422
指導教授: 管一政
學位類別: 碩士
Master
系所名稱: 地球科學系
Department of Earth Sciences
論文出版年: 2010
畢業學年度: 98
語文別: 中文
論文頁數: 87
中文關鍵詞: 天文化學有機分子低質量原恆星
論文種類: 學術論文
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  • 我們使用SMA次毫米波干涉陣列觀測低質量原恆星雙星系統IRAS 16293-2422。在次角秒解析度下(0.9〃× 0.5〃),可以解析出I16293A有三個明顯的連續積分強度位置,而I16293B仍是一個未解析的點源。多數含硫分子存在於天體I16293A,且光譜結構複雜,暗示含硫分子在天體I16293A附近有著複雜的氣體動力結構。在角秒解析度(3.3〃× 1.2〃)的觀測裡,包含基態與扭轉激發態的CH3OH分子,多數分子有明顯的藍移與紅移速度組成的光譜輪廓,從基態CH3OH分子所計算出的旋轉激發溫度為261 K(I16293A)和211 K(I16293B)。另一方面,C2H5OH分子與CH3CHO分子所得到的旋轉激發溫度分別為214 K(I16293A) 與313 K(I16293B),暗示在低質量恆星形成區也存在高溫的分子形成環境與種類豐富的有機分子,也間接證實了低質量熱分子雲核hot corinos的存在。我們在I16293A與I16293B上分別觀測到C2H5OH及CH3CHO分子有不同的空間分布,顯示出這兩個天體有不同的演化時期。其他複雜的有機分子,所得的旋轉激發溫度都大於150 K,甚至在I16293B上的34SO2分子有350 K,表示無論在I16293A或I16293B上都有高溫的分子形成區域。另外比較彼此之間的豐度比例,發現有許多分子的豐度並無法與化學模型有一致結果,暗示低質量恆星形成區裡分子形成過程可能與高質量熱分子雲核在化學途徑演化上有著顯著的差異。

    摘要 I 目次 II 圖目 IV 表格 VI 第一章 緒論 1 1.1 星際介質與分子雲 1 1.2 低質量原恆星的演化 2 1.3 低質量Class 0原生恆星源:IRAS 16293-2422 3 第二章 觀測與資料處理 7 2.1 SMA望遠鏡 7 2.2 347-GHz觀測 7 2.3 353-GHz觀測 8 第三章 結果 13 3.1 347-與353-GHz之連續發射光譜 13 3.2 複雜的有機分子 17 3.3 含硫分子 21 3.4 其它簡單的分子 22 第四章 醇類及乙醛分子的分析與討論 31 4.1 分子氣體旋轉激發溫度與柱密度的計算 31 4.2 353-GHz CH3OH的光譜 32 4.3 337/347-GHz的 CH3OH分子 38 4.3.1 影像與光譜 38 4.3.2 基態躍遷態的CH3OH分子(υt = 0) 38 4.3.3 激發躍遷態的CH3OH分子(υt = 1) 39 4.3.4 激發躍遷態的CH3OH分子(υt = 2) 40 4.3.5 CH3OH分子的旋轉激發溫度與柱密度 40 4.4 C2H5OH分子 47 4.4.1 C2H5OH分子的早期觀測 47 4.4.2 C2H5OH分子的積分影像與光譜 48 4.5 CH3CHO分子 49 4.5.1 CH3CHO分子過去的觀測 49 4.5.2 CH3CHO分子的積分影像與光譜 55 4.5.3 CH3CHO與C2H5OH分子的關係 56 第五章 其它分子的分析與討論 58 5.1 低質量恆星形成區的化學反應區域 58 5.2 其他分子 59 5.2.1 C2H5CN分子 59 5.2.2 HCOOH分子 61 5.2.3 CH3OCH3分子 62 5.2.4 CH3OCHO分子 63 5.2.5 SiO分子 65 5.2.6 未鑑定的光譜線 70 5.3 各分子間的豐度比較 70 5.4 化學模型的解釋 76 第六章 總結 78 參考文獻 81 附錄:分子光譜資料庫簡介 86

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