以天文光譜量測技術研究源自DG Tau A的低速風

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研究生：	周育如 Chou, Yu-Ru
論文名稱：	以天文光譜量測技術研究源自DG Tau A的低速風 A Spectroastrometric Study of the Low-velocity Wind from DG Tau A
指導教授：	賴詩萍 Lai, Shih-Ping 高見道弘 Takami, Michihiro
口試委員:	平野尚美 Hirano, Naomi 李景輝 Lee, Chin-Fei
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：	2024
畢業學年度：	112
語文別：	英文
論文頁數：	63
中文關鍵詞：	原行星盤、觀測天文學、盤面風、噴流、電漿診斷
外文關鍵詞：	protoplanetary-disk, wind, jet, observation, diagnostics
相關次數：	點閱：65 下載：3
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可見光禁制線（optical forbidden line）的低速成分（low-velocity component,
LVC, |v| < 100 km s−1）常被詮釋為原行星盤面風（protoplanetary disk wind）。
原行星盤面風對於原行星盤消散具有潛在的影響力，而我們的目的在於藉由研究LVC理解原行星盤面風的物理性質。我們以Subaru-HDS觀測DG Tau A並取得了23條可見光禁制線（[N I], [N II], [O I], [O II], [O III], [S II], [Ca II], [Fe II]）的高解析度光譜（Δv ∼ 2.5 km s−1），其波長範圍為4800 Å至7500 Å，涵蓋3條容許譜線（permitted line；Hα, Hβ, He I）。而LVC則在[O I] 5577、6300、6364 Å、[S II] 6716、6731 Å譜線被觀測到。我們對於LVC的分析結果指出其可被分解為三個子成分：LVC-H、LVC-M和LVC-L。以上三個成分分別可解釋為紊流、廣角盤面風（wide-angled wind），以及上層盤面大氣（upper disk atmosphere）。我們以光譜天文量測技術（spectroastrometry）測出盤面風的長度為12-70 au，並估算出其質量流失率（wind mass-loss rate）之最低值為約10^−8 M⊙ yr−1。我們的觀測結果與現有的三種盤面風模型：光蒸發風（photoevaporative wind）、D-wind、X-wind模型之間的比較表明，需要嘗試組合不同模型並對其進行廣泛的模擬觀測（synthetic observation），以辨明盤
面風的驅動機制。除了三個LVC之外，我們在全部26條譜線中皆鑑別出一或兩個高速成分（HVCs, |v| > 100 km s−1）。其中，在下游處的高速成分距離中心星約1"，其密度約為10^4 cm−3，皆與過去的DG Tau A噴流之內部衝擊面（internal shock surface）研究結果相符。而靠近中心星的高速成分距離中心星約0".06 - 0".25，符合過去對於DG Tau A之駐震波（stationary shock）的觀測結果。

Low-velocity components (LVCs, |v| < 100 km s−1) in optical forbidden line profiles are used as a proxy for protoplanetary disk winds. We aim to study the line properties of LVCs that potentially affect disk dispersal. Using Subaru-HDS, we obtained high spectral resolution spectra (Δv ∼ 2.5 km s−1) for DG Tau A and detected 23 optical forbidden lines ([N I], [N II], [O I], [O II], [O III], [S II], [Ca II], [Fe II]) from 4800 Å to 7500 Å and also three permitted lines (Hα, Hβ, He I). Among these lines, LVCs were observed in the [O I] 5577, 6300, 6364 Å, [S II] 6716, 6731 Å lines. Our analysis reveals that the LVCs can be divided into three subcomponents: LVC-H, LVC-M, and LVC-L. These components may trace turbulent gas, a wide-angled wind, and an upper disk atmosphere, respectively. With 12-70 au wind lengths measured using spectroastrometry, we estimate a lower limit to the wind mass-loss rate of ∼10^−8 M⊙ yr−1. Comparisons between our observation and available photoevaporative wind, D-wind, and X-wind models suggest the need for more extensive synthetic observations of combined wind models to identify the driving mechanism. In addition to the LVCs, we identified one or two high-velocity components (HVCs, |v| > 100 km s−1) associated with the collimated jet in all 26 lines. The one downstream (∼1", ne ∼10^4 cm−3) is associated with an internal shock surface, while the other at the base (0".06 - 0".25) may be a stationary shock component.

Abstract (Chinese) I
Abstract II
Acknowledgements (Chinese) III
Contents V
List of Figures VII
List of Tables XIII
1 Introduction 1
1.1 Disk winds . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2
1.2 Wind launching mechanisms . . . . . . . . . . . . . . . . . . . . . . 3
1.3 Previous observations of the winds . . . . . . . . . . . . . . . . . . 4
1.4 DG Tau A . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6
2 Observations and Data Reduction 11
3 Results 14
3.1 Overview of the emission lines properties . . . . . . . . . . . . . . . 14
3.2 Major target lines . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19
4 Physical Conditions and Nature of Individual Emission Components
27
4.1 Calculations using ChiantiPy and Pyneb . . . . . . . . . . . . . . . 27
4.2 The origin of the HVCs . . . . . . . . . . . . . . . . . . . . . . . . . 28
4.3 The low-velocity components (LVCs) . . . . . . . . . . . . . . . . . 32
5 Driving Mechanism for the LVC-M Wind 40
5.1 Comparisons with the PE and D-wind models . . . . . . . . . . . . 40
5.1.1 PE wind . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41
5.1.2 D-wind . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41
5.1.3 PE + D-wind . . . . . . . . . . . . . . . . . . . . . . . . . . 42
5.1.4 PE wind with Lamppost Illumination . . . . . . . . . . . . . 43
5.2 Comparisons with the X-wind model . . . . . . . . . . . . . . . . . 44
6 Summary 46
Bibliography 49
A [O I] 5577 Å position spectra 57
B Search for the LVC in Other Emission Lines 59
B.1 [N I] 5200 Å . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 59
B.2 [Ca II] 7291 Å . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 61
B.3 [O III] 5007 Å . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62
B.4 [O III] 4959 Å . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62
                                

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