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研究生: 王俊捷
Wang, Chun-Chieh
論文名稱: 漸近巨星分支星中含碳量高之環星包層HC3N(J=5-4)分子轉動譜線的高解析影像觀測
High Resolution Imaging of HC3N (J=5-4) Emission from Carbon Rich Envelopes of Asymptotic Giant Branch Stars
指導教授: 賴詩萍
Lai, Shih-Ping
丁文忠
Dinh Van Trung
口試委員:
學位類別: 碩士
Master
系所名稱: 理學院 - 天文研究所
Institute of Astronomy
論文出版年: 2007
畢業學年度: 95
語文別: 英文
論文頁數: 38
中文關鍵詞: 漸近巨星分支環星包層分子碳星譜線質量損失
外文關鍵詞: AGB, circumstellar envelope, molecule, carbon star, emission line, mass-loss
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  • 本論文中,我們探討從五個含碳量高的漸近巨星分支星的環星包層所發射出來的HC3N (J=5-4)分子轉動譜線觀測結果。觀測目標包含LP And,V Cyg,IRAS 22272+5435,V384 Per及RAFGL 2155。我們使用Very Large Array針對7毫米波段(45490.3 MHz)作觀測。我們獲得約1.5角秒的高解析度足夠讓我們解析出HC3N在環星包層中的分布為中空球殼狀結構。如此的分布與先前由其他漸近巨星分支星的環星包層所做出的HC3N分子形成之化學模型吻合。不過我們仍發現有些許成塊狀或是長條狀等不對稱分布。另外我們還發現環星包層的大小與中心星球的質量損失率有關。我們高解析的觀測結果為現階段含碳量高之環星包層的化學模型提供了非常有用的限制條件。


    In this thesis, we investigated the HC3N (J=5-4) emission at 45490.3 MHz from the circumstellar envelopes of five carbon rich stars (LP And, V Cyg, IRAS 22272+5435, V384 Per, RAFGL 2155). The observations were carried out using the Very Large Array of the National Radio Astronomical Observatory. The high angular resolution of ∼1”.5 allows us to resolve the distribution of HC3N in these envelopes into hollow shell structure in constant expansion. Such distribution is in broad agreement with prediction of chemical models on the formation of HC3N molecules. We also find that the distribution of HC3N is clumpy and in a few cases asymmetric. Interestingly, we find a clear relation between mass loss rate from the central star and the linear size of the envelope. Our results provide very useful constraints to the current chemical models for the carbon rich envelope.

    List of Figures .............................. iii List of Tables .............................. v 1 Introduction .............................. 1 2 Observations and Data Reduction ................... 8 2-1 Sources ................................ 8 2.1.1 LP And .............................. 8 2.1.2 V Cyg .............................. 8 2.1.3 IRAS 22272+5435 ......................... 9 2.1.4 V384 Per ............................. 10 2.1.5 RAFGL 2155 ............................ 10 2.2 Observations ............................. 11 2.3 Data Reduction ............................ 12 3 Observational results ......................... 15 3.1 LP And ................................ 15 3.2 V Cyg ................................ 18 3.3 IRAS 22272+5435 ........................... 21 3.4 V384 Per ............................... 21 3.5 RAFGL 2155 .............................. 26 4 Analysis ................................ 29 4.1 Column Density of HC3N Molecule ................... 29 4.1.1 Radiative Transfer ........................ 29 4.1.2 Derivation of Column Density ................... 30 4.1.3 Comparison of IRC +10216 .................... 32 4.2 The Structure of Envelope ....................... 33 4.2.1 The relation between mass-loss rate and the size of envelope ...... 33 4.2.2 Clumps and asymmetrical distribution ................ 34 5 Conclusion............................... 35 References ................................ 36 References ................................ 36

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