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http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/18784Full metadata record
| ???org.dspace.app.webui.jsptag.ItemTag.dcfield??? | Value | Language |
|---|---|---|
| dc.contributor.advisor | 賀曾樸(Paul Ho),李景輝(Chin-Fei Lee) | |
| dc.contributor.author | Hung-Jin Huang | en |
| dc.contributor.author | 黃虹瑾 | zh_TW |
| dc.date.accessioned | 2021-06-08T01:25:50Z | - |
| dc.date.copyright | 2014-08-01 | |
| dc.date.issued | 2014 | |
| dc.date.submitted | 2014-07-31 | |
| dc.identifier.citation | Beckwith, S. V. W. and Sargent, A. I. (1991). Particle emissivity in circumstellar disks. Astrophys. J., 381:250--258.
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/18784 | - |
| dc.description.abstract | IRAS 4A2 是一顆在Class 0 階段的低質量原恆星，位於英仙座星團中的NGC1333分子雲裡面，距離地球大約是235秒差距。之前的許多觀測顯示，在這顆原恆星有偵測到inverse P-Cygni特徵的光譜，因此IRAS 4A2目前被認定很可能正有坍縮運動發生；除了坍縮運動外，旋轉及噴流運動也有被觀測到。在這個研究裡，我們利用高解析度的次毫米波望遠鏡觀測，以及建立輻射轉移的模型，去分析這些觀測到的氣體運動。在結合Compact-North，Extended，以及Very-Extended三種陣型的次毫米波觀測資料後，我們也在13CO J=2-1 這條譜線看到了有inverse P-Cygni特徵的光譜，也看到了在光譜紅移的波段裡，有很深的吸收現象。在建立輻射轉移模型的過程中，我們發現以一個正在坍縮的球體、在球體內部放入一緻密扁平狀的原恆星盤、以及一大片在原恆星前以8 km/s速度前進的冷氣體雲，可以用來模擬出觀測到的13CO J=2-1光譜和其位置-速度圖(PV diagram)。由輻射轉移模型計算出的結果顯示，IRAS 4A2是一個處在高速坍縮階段的系統，其單位時間的坍縮質量數量級大約在10^-4 M☉/yr。而位在其中心，尚未被解析出的原恆星盤大小約為20 AU，其質量大約為0.02 M☉。 | zh_TW |
| dc.description.abstract | IRAS 4A2 is a nearby, Class 0 low-mass protostellar system residing in the NGC 1333 molecular cloud in Perseus cluster. With detections of inverse P-Cygni profile, this target has been identified as a good infall candidate in several studies. Motions of outflow and rotation have also been observed. We decompose these different gas motions in aids of high resolution SMA observation and through radiative transfer modeling. Combining Compact-North, Extended and Very Extended configuration data from SMA, an inverse P-Cygni line profile together with a wide and strong absorption dip over a broad range of area is seen toward 4A2 in 13CO J=2-1 . From our radiative transfer modeling, an infalling envelope with a compact disk structure inside, together with a foreground cold layer at around 8 km/s can be used to interpret the observed spectrum and PV diagram of 4A2. We derive a high mass infall rate of an order of 10^-4 M☉/yr in the envelope. The unresolved disk component is roughly constrained to be 20 AU in radius and 0.02 M☉ in mass. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-08T01:25:50Z (GMT). No. of bitstreams: 1 ntu-103-R01244004-1.pdf: 1732497 bytes, checksum: 0634f1d5cbee4e3cdad8425f8615f96e (MD5) Previous issue date: 2014 | en |
| dc.description.tableofcontents | Contents
口試委員會審定書 i 致謝 ii 中文摘要 iii Abstract iv Contents v List of Figures vii List of Tables viii 1 Introduction 1 2 Observations and Data reduction 4 2.1 Observations ................................ 4 2.2 DataReductionandImaging ........................ 5 3 Observational Results 6 3.1 DustContinuumEmission ......................... 6 3.2 13COJ=2-1................................. 7 4 Radiative Transfer Modeling 13 4.1 ModelStructure............................... 13 4.2 ModelResult ................................ 18 5 Discussions 27 5.1 The Origin of the Inverse P-Cygni Profile toward IRAS 4A2 . . . . . . . 27 5.2 TheDiskSizeof4A2............................ 28 5.3 MassInfallRatetoward4A2........................ 29 6 Conclusions 31 Bibliography 33 | |
| dc.language.iso | en | |
| dc.title | 原恆星 NGC 1333 IRAS4A2 的氣體運動 | zh_TW |
| dc.title | The gas motions around the protostar NGC 1333 IRAS4A2 | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 102-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 呂聖元(Sheng-Yuan Liu) | |
| dc.subject.keyword | 恆星形成,原恆星盤,坍縮運動,吸積, | zh_TW |
| dc.subject.keyword | star formation,protostellar disk,infall motion,accretion, | en |
| dc.relation.page | 36 | |
| dc.rights.note | 未授權 | |
| dc.date.accepted | 2014-07-31 | |
| dc.contributor.author-college | 理學院 | zh_TW |
| dc.contributor.author-dept | 天文物理研究所 | zh_TW |
| Appears in Collections: | 天文物理研究所 | |
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| File | Size | Format | |
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| ntu-103-1.pdf Restricted Access | 1.69 MB | Adobe PDF |
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