博碩士論文 110229005 詳細資訊



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姓名 陳湘喻(Hsiang Yu Chen)  查詢紙本館藏   畢業系所 天文研究所
論文名稱
(The Young Stellar Population in the Chamaeleon-Musca Dark Cloud Complex)
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摘要(中) 內容. 蝘蜓—蒼蠅座分子雲的低質量恆星形成區距離太陽約 200 秒差距。前人
文獻已經多次普查這些年輕恆星族群，但研究的範圍幾乎只聚焦在分子雲本
身。
目標. 為了診斷蝘蜓—蒼蠅座分子雲的恆星形成歷史，我們除了尋找在分子雲
上的年輕成員星之外，也調查雲以外的區域。
方法. 我們研究比前人文獻廣上許多的區域12◦ × 12◦，利用 Gaia DR3 提供
的高度精確測光以及天體測量數據，加上近紅外波段 2MASS 與中紅外波段
ALLWISE 的顏色，尋找年輕恆星成員。
結果. 我們確認蝘蜓 I 的恆星形成是這個區域中最活躍的，有近 200 顆的年輕
恆星成員。蝘蜓 II 擁有 50 幾顆年輕恆星，而其中三顆位在蝘蜓 III 的北邊，但
蝘蜓 III 本身沒有自己的恆星形成。蒼蠅座分子雲也沒有年輕恆星，但根據文獻
它孕育了原恆星核，表示正處於誕生恆星的前期狀態。Cha I 的成員可以從距
離分為南邊 189−5
+5 秒差距與北邊 193−3
+2 秒差距，而 Cha II 的成員星大約落在
197−5
+5 秒差距，這兩個年輕恆星族群的年齡大約是三百萬年。位在我們研究的
恆星形成區的前景(約 110 秒差距)，我們找到一些 ε Cha 和下半人馬-南十字座
的星協成員，他們是演化更久的年輕恆星或是主序星，年齡分佈廣從五百萬至
兩千萬年。
總結. 在分子雲裡的已知成員星，與我們新找到的雲外的成員星，有一致的距
離與年齡，推測這可能是附近的 OB 星協影響蝘蜓—蒼蠅座分子雲的恆星誕
生。
摘要(英) Context. The Chamaeleon-Musca dark cloud complex is a known low-mass
star-forming region at a distance of ∼200 pc. The young stellar populations
have been investigated in previous works, but mostly focused toward the main
clouds.
Aims. We searched for young members not only associated with the main
clouds but also in intercloud regions in order to diagnose the star formation
history of the entire complex.
Method. By using Gaia DR3 data, which provide unprecedentedly precise
photometry and astrometry for membership, and near- and mid-infrared photometry from 2MASS and ALLWISE for stellar youth, we investigate a sky area
of 12◦ × 12◦
toward the cloud complex, much larger than previously reported in
the literature.
Results. We confirm that Cha I is active in star formation, with nearly 200
young members. There are more than 50 young members in Cha II, among
which three are projected in northern Cha III which itself lacks any star-forming
activity. The Musca cloud harbors no young star, though it is known to host
prestellar cores. Cha I indeed as known has two subclusters, with the northern
group at 193+2
−3 pc and the southern group at 189+5
−5 pc. Cha II is at 197+5
−5 pc,
and has an age of about 3 Myr as in Cha I. Some members of ϵ Cha and Lower
Centaurus-Crux associations projected in the foreground (∼110 pc) toward our
studied region are found to be evolved young stars or dwarfs, with a wide age
spread of ∼5–20 Myr.
Conclusions. Our reliable sample of young stellar members provides accurate diagnosis of distance, age, and their relation to parental molecular clouds,
including those already known in the literature, plus a few newly found offcloud members, suggesting a coeval star formation likely influenced by nearby
OB stars.
Thesis Supervisor: Wen-Ping Chen
Title: Professor
關鍵字(中) ★ 恆星形成
★ 分子雲
★ 蝘蜓座分子雲
★ 蒼蠅座分子雲
★ Epsilon Cha 星協		 關鍵字(英) ★ star formation
★ molecular cloud
★ Chamaeleon
★ Musca
★ Epsilon Cha
論文目次 Contents
1 Introduction 1
1.1 Star Formation and Young Stellar Objects . . . . . . . . . . . . . . 1
1.2 The Chamaeleon-Musca Dark Cloud Complex . . . . . . . . . . . 2
2 Data Sources and Analysis 9
2.1 Individual Cloud Regions . . . . . . . . . . . . . . . . . . . . . . . 10
Cha I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
Cha II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15
Cha III . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 16
Musca . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19
2.2 The 12◦ × 12◦ Field of the Complex at Large . . . . . . . . . . . . 21
ϵ Cha Association . . . . . . . . . . . . . . . . . . . . . . . . 22
Cha I and Cha II . . . . . . . . . . . . . . . . . . . . . . . . 24
3 Results and Discussions 27
3.1 Cha I . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 27
3.2 Cha II . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 32
3.3 Proper motion, Distance, and Age of Each Cloud . . . . . . . . . . 36
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指導教授 陳文屏(Wen-Ping Chen) 審核日期 2024-7-9
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