對於年輕恆星體中的塵埃，何時會從（次）微米尺度的星際塵埃，生長到毫米尺度的隕石球粒，目前尚未有定論。先前的研究基於在（次）毫米波段觀察到較低的光譜指數（~2-3），普遍認為塵埃在早期（如第0/I期）的年輕恆星體中已經長到毫米大小。如果確實如此，在（次）毫米觀察到的偏極光，則有可能是經由塵埃散射所發出的線偏振散射光，而不是藉由非球形塵埃受到磁性影響會傾向整齊排列的特性，所發出的線偏振發射光。釐清這個議題，不僅對於瞭解塵埃顆粒的生長和類地行星的形成至關重要，也會對原行星盤形成和演化的研究產生影響。

本研究的主要目標是檢驗我們的假設：（一）在第0/I期的年輕恆星體中，最大的塵埃顆粒小於100微米。（二）先前的觀測結果檢測到低光譜指數的主要原因是：原行星（假）盤在次毫米波長下有較高的光學深度，以及其溫度會隨半徑增加而下降。（三）塵埃的長軸與磁場的方向垂直。（四）在原行星（假）盤上，（次）毫米偏極光是來自於塵埃的線偏振二向色性消光；在包覆原恆星的氣體團中（~500到1000天文單位），偏極光則是來自塵埃的線偏振發射光。

本研究使用卡爾·央斯基甚大天線陣列（JVLA）和阿塔卡瑪大型毫米波及次毫米波陣列（ALMA），對年輕第0期的雙星系統NGC1333 IRAS4A，進行多波段、高解析度的塵埃偏極光觀測。我們利用JVLA的觀測結果首次在7至17毫米波長（18至48十億赫茲）成功檢測到年輕恆星體的塵埃線偏振光。透過將這些JVLA的觀測與ALMA在0.87、1.3和2毫米波長處的觀測進行比較，我們首次明確地驗證了塵埃二向色性消光在這些波段下的特性，並進而重新解釋磁場的型態。最後，基於在視線方向上的兩個塵埃組成的簡化模型，我們初步得出：在~60至1000天文單位的尺度上，觀測到的塵埃連續體強度、偏振強度以及偏振角度，與最大塵埃顆粒小於100微米的假設相符。

When dust grains grow from (sub)micron-sized interstellar dust to millimeter-sized chondrules in young stellar objects (YSOs) remains under debate. Based on the observations of the low spectral indices (~2-3) at the (sub)millimeter wavelengths, previously, it had been generally considered that dust grains have already grown to millimeter sizes during the embedded stages (i.e., Class 0/I) of YSOs. If this is indeed the case, then the (sub)millimeter polarization observations may trace the linearly polarized dust scattered light instead of the linearly polarized emission of the non-spherical dust grains which are presumably aligned with the magnetic field. Clarifying this issue is not only crucial to our understanding of grain growth and terrestrial planet-formation but will also impact on the investigation of protoplanetary disk formation and evolution.

The main subject of this study is to test our alternative hypotheses: (1) the maximum dust grain sizes in Class 0/I YSOs remain smaller than 100 microns, (2) the embedded protoplanetary (pseudo-)disks are optically thick at the submillimeter wavelengths and present radially decreasing temperature profile, which are the main reasons why the previous observations detected low spectral indices, (3) the projected long axis of dust grains are aligned perpendicular to the magnetic field, and (4) at the projected areas of the protoplanetary (pseudo-)disks, the (sub)millimeter polarization observations trace the linearly polarized dichroic dust extinction; they trace the linearly polarized dust emission at the projected areas of the spatially extended (~500-1000 au) circumstellar envelopes.

Our research is based on the high angular resolution, multi-wavelength observations of dust polarization towards the Class 0 protobinary system, NGC1333 IRAS4A, using the Karl G. Jansky Very Large Array (JVLA) and the Atacama Large Millimeter Array (ALMA). Our JVLA observations yielded the first successful detection of dust linear polarization at 7-17 mm wavelengths (18-48 GHz). By comparing these JVLA observations with the ALMA observations at 0.87, 1.3, and 2 mm wavelengths, we have unambiguously verified the characteristic signatures of the polarized dichroic dust extinction at these wavelengths for the first time. This result has forced a re-interpretation of the magnetic field topology. Finally, based on a simplified model with two dust components in a line-of-sight, we tentatively conclude that the observed Stokes $I$ intensities, polarized intensities, and polarization position angles are consistent with the less than 100-micron maximum grain sizes on ~60-1000 au scales.

Abstract ......................................................... i
摘要 .............................................................. ii
致謝 .............................................................. iv
List of Figures .................................................. x
List of Tables ................................................... xii

1. Introduction .................................................. 3
1.1. Star Formation Overview ..................................... 3
1.1.1. Probing Star Formation: Planck function ................... 3
1.1.2. Classification of Young Stellar Objects ................... 4
1.2. Open Question: When do Dust Grains Growth from (Sub)micron Size to Millimeter Size in Young Stellar Objects? ..................... 6
1.2.1. One Approach to the Question: Dust Opacity Spectral Index . 7
1.2.2. Another Approach to the Question: Dust Self Scattering .... 8
1.2.3. Previous Studies: Dust Grain Growth in YSOs ............... 9
1.2.4. A Case Study of NGC1333 IRAS4A ............................ 9
1.3. Open Question: What Role do Magnetic Fields Play in the Process of Star Formation? ............................................... 11
1.3.1. One Approach to the Question: Magnetic Field Morphology ... 12
1.3.2. Previous Studies: Magnetic Field Morphology in YSOs ....... 13
1.3.3. A Case Study of NGC1333 IRAS4A ............................ 15
1.4. Motivation .................................................. 15
1.4.1. Why do We Use JVLA and ALMA? .............................. 16
1.4.2. Why do We Observe Dust Polarization? ...................... 16
1.4.3. Why do We Observe NGC1333 IRAS4A? ......................... 17
1.5. OverviewoftheThesis ......................................... 17

2. Multi-Wavelength Dust Polarization Observations toward NGC1333 IRAS4A with JVLA and ALMA: Resolving Polarization Mechanisms ..... 19
2.1. Introduction ................................................ 20
2.1.1. Motivation ................................................ 20
2.1.2. Target Source ............................................. 21
2.1.3. Overview of this Section .................................. 21
2.2. Observations and Data Reduction ............................. 22
2.2.1. JVLA Observations ......................................... 22
2.2.2. ALMA Observations ......................................... 22
2.2.3. Polarization Images ....................................... 23
2.3. Results ..................................................... 25
2.3.1. Polarization Position Angle ............................... 25
2.3.2. Polarization Percentage ................................... 25
2.4. Discussion .................................................. 28
2.4.1. Inferred Magnetic Field Morphology at the Scale of 100–1000 AU
around IRAS4A .................................................... 28
2.4.2. Derived Optical Depth at the Inner 100 AU of IRAS4A1 ...... 28
2.4.3. Polarization Mechanism .................................... 30
2.4.3.1. Dust Self-Scattering? ................................... 30
2.4.3.2. Radiative Alignment? .................................... 31
2.4.3.3. Dust Grains Aligned with Magnetic Field ................. 31
2.4.4. Toy Model to Interpret the Trends of Polarization Percentage .................................................................. 31
2.5. Conclusions ................................................. 33

3. Astrometry: Proper Motion and Parallax of NGC1333 IRAS4A ...... 35
3.1. Introduction ................................................ 35
3.1.1. Motivation ................................................ 35
3.1.2. Formulae of the Proper Motion and the Parallax ............ 35
3.1.3. Overview of this Section .................................. 36
3.2. Observations and Data Reduction ............................. 36
3.3. Data Analysis Procedures .................................... 38
3.3.1. Source Position ........................................... 38
3.3.2. Astrometric Accuracy ...................................... 38
3.3.3. Astrometry Fitting ........................................ 38
3.4. Results ..................................................... 39
3.5. Discussion and Conclusions .................................. 42

4. Dual-Wavelength Dust Polarization Observations toward NGC1333 IRAS4A with ALMA at High Angular Resolution ...................... 43
4.1. Introduction ................................................ 44
4.1.1. Motivation ................................................ 44
4.1.2. Overview of this Section .................................. 44
4.2. Observations and Data Reduction ............................. 44
4.2.1. Polarization Observations ................................. 44
4.2.2. Polarization Images ....................................... 45
4.3. Results ..................................................... 46
4.3.1. Dust Stokes I Continuum Emission .......................... 47
4.3.1.1. Morphology .............................................. 47
4.3.1.2. Brightness Temperature .................................. 47
4.3.1.3. Spectral Index .......................................... 51
4.3.2. Dust Polarization toward IRAS4A1 .......................... 51
4.3.3. Dust Polarization toward IRAS4A2 .......................... 52
4.4. Analysis .................................................... 52
4.4.1. General Description of our Toy Model ...................... 52
4.4.2. One-Component Model toward IRAS4A2 ........................ 54
4.4.3. Two-Component Model toward IRAS4A1 ........................ 54
4.5. Discussion .................................................. 55
4.5.1. Stokes I Intensity ........................................ 55
4.5.2. Polarization Angle ........................................ 56
4.5.3. Polarization Percentage ................................... 57
4.5.4. Possible Evidence for Candidate Disk in IRAS4A1 ........... 57
4.5.5. Inferred Magnetic Field Morphology ........................ 58
4.6. Conclusions ................................................. 59

5. Conclusions and Future Prospects .............................. 69
5.1. Thesis Conclusions .......................................... 69
5.2. Future Prospects ............................................ 71

A. Appendix to Chapter 2 ......................................... 73
A.1.Polarization Measurements .................................... 73
A.2.Polarization Images .......................................... 73
B. Appendix to Chapter 3 ......................................... 77
B.1. One Dimensional Slice of Stokes I Intensity in IRAS4A1 and IRAS4A2 .......................................................... 77
B.2. Stokes I Images in IRAS4A1 and IRAS4A2 at Different Epochs .. 77
C. List of Mathematical Symbols .................................. 93
D. List of Abbreviations ......................................... 95

Bibliography ..................................................... 97

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