蛇夫座ρ星雲複合體心宿增四恆星形成區域中分子雲與年輕恆星的交互作用;Interplaying Between Young Stars and Molecular Clouds in the Rho Ophiuchi Star-Forming Complex

Please use this identifier to cite or link to this item: http://ir.lib.ncu.edu.tw/handle/987654321/85683

Title:	蛇夫座ρ星雲複合體心宿增四恆星形成區域中分子雲與年輕恆星的交互作用;Interplaying Between Young Stars and Molecular Clouds in the Rho Ophiuchi Star-Forming Complex
Authors:	阿市社;Gupta, Aashish
Contributors:	天文研究所
Keywords:	恒星形成;Star Formation
Date:	2021-03-25
Issue Date:	2021-12-07 11:14:49 (UTC+8)
Publisher:	國立中央大學
Abstract:	大部分在星系團中的新形成恆星被淹沒在巨大分子雲當中，這些系統是研究恆星形成的宏觀物理的自然實驗室。其中一種可以理解恆星形成歷史的方法是同時研究其中年輕恆星以及他們所在的分子雲。在138秒差距外的蛇夫座ρ星雲複合體有著高度氣體集中，且其中星體普遍在幼兒年紀(1-2百萬年)，是作為研究良好的目標透過JCMT/SCUBA-2 850微米的影像，我們追蹤分子雲在蛇夫座ρ星雲複合體中心高密度區域的形象學。另外一方面，我們透過Gaia/eDR3的資料新增了4個在蛇夫座ρ星雲複合體的年輕星際星體。利用這些資料集，我們分析了這些年輕星際族群在不同演化階段上相對不同氣體結構的空間與移動的關係我們發現演化到後期的星體傾向疏散，遠離氣體，且他們的運動暗示著他們誕生於原本的地方而後驅散了周遭氣體。而且我們分析過後，這個年輕星團正處於初步塌縮階段，而低質量核心很可能是快速移動的族群。;Most stars form in clusters embedded in giant molecular clouds and these systems are natural laboratories to study macrophysics of star formation. One way to get a comprehensive view of their star formation history is to concurrently study the two major components of these regions: young stellar objects (YSOs) and their natal molecular clouds. The $\rho$ Ophiuchus cloud complex, with its proximity ($\sim$138 pc) and a high concentration of gas and stellar population in infancy (1-2 Mys), is an excellent target for such a study. Using the deepest 850$\mu$m JCMT/SCUBA-2 image of the densest core of $\rho$ Ophiuchus, generated as part of the JCMT Transient Survey, we trace the morphology of molecular clouds in the region. On the other hand, we also compiled a catalogue of YSOs in the region using published lists in literature and four more members, identified using the Gaia/eDR3 astrometric data. Using these datasets, we diagnosed the spatial and kinematic correlation of the young stellar population, at different evolutionary stages, with respect to the gaseous structures. We found that the more evolved sources tend to be scattered further away from clouds and their kinematics suggest that they were formed in-situ and have dispersed the surrounding gas. Moreover, our analysis suggests that the young cluster is in the initial collapse phase and low mass cores are, likely, a faster-moving population.
Appears in Collections:	[Graduate Institute of Astronomy] Electronic Thesis & Dissertation

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