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恆星形成

Kinematic properties of velocity-decomposed [Ne III] λ3869 emission are shown in a position–velocity (pv) diagram (left panel), a spatial profile along the jet axis (central panel), and line profiles at specific spatial positions (right three panels). In the pv diagram, the decomposed high-velocity component (HVC) and low-velocity component (LVC) are shown by green and red contours, respectively. The yellow symbols represent the HVC velocity centroids and orange symbols represent the LVC velocity centroids. The spatial profile is shown on a logarithmic scale to accommodate the large contrast between the innermost 3'' emission and the outer knots.
The [Ne III] Jet of DG Tau and Its Ionization Scenarios
Kinematic properties of velocity-decomposed [Ne III] λ3869 emission are shown in a position–velocity (pv) diagram (left panel), a spatial profile along the jet axis (central panel), and line profiles at specific spatial positions (right three panels). In the pv diagram, the decomposed high-velocity component (HVC) and low-velocity component (LVC) are shown by green and red contours, respectively. The yellow symbols represent the HVC velocity centroids and orange symbols represent the LVC velocity centroids. The spatial profile is shown on a logarithmic scale to accommodate the large contrast between the innermost 3'' emission and the outer knots.
The [Ne III] Jet of DG Tau and Its Ionization Scenarios
2D slices through the centre of the 3D domain of our simulations. Panel (a) shows log of density of our steady jet velocity simulation. It can be directly compared to (b) showing log of density of the 170 ± 20 km/s velocity simulation. The remaining panels show the velocity (c), log of temperature (d), and H2 fraction (e), of the 170 ± 20 km/s velocity simulation. The wiggle-shaped trajectory from the orbital motion, combined with the jet beam velocity pulsations lead to progressively angled internal or ‘oblique’ shocks. Blue lines in the H2 fraction plot are drawn to illustrate the orientation of these oblique shocks in the displayed 2D plane.
A study of the wiggle morphology of HH 211 through numerical simulations: View of the simulation
Top panel: a reproduction of fig. 1(b) from Lee et al. (2010) showing the CO emission integrated intensity map of HH 211 within 17 arcsec from the source. The red and blue contours highlight the redshifted and blueshifted components integrated from 20 to 43 km/s and −16 to 0 km/s, respectively, where the contours begin at 0.56 Jy/beam km/s and step at intervals of 0.84 Jy/beam km/s. The location of the blueshifted and redshifted knots are labelled. The red and blue lines trace the wiggle produced by the analytical model. Second panel: simulated synthetic CO emission map for the steady velocity jet simulation. For a direct comparison to the observation, it uses the same channel map velocity range and contour intensity values. The green line traces the analytical model wiggle. This shows that the assumption of the jet source in a binary system can indeed reproduce the reflection symmetric wiggle. Third panel: simulated synthetic CO emission map of the 170 ± 20 km/s pulsed jet simulation. Again the channel map velocity range and contour intensity values are the same as the observational image and the green line traces the analytical model wiggle. We see that whereas the observational map has intense jet emission near the jet source, the simulated map has weaker emission near the source. Also, the positions of the knots are not precisely aligned with the positions of the observational knots, especially in the blueshifted side. However, the intensity range of the simulated knots are similar to the observational knots. Fourth panel: similar to the third panel, but for the 170 ± 50 km/s pulsed jet simulation. Note, the displayed time is at an earlier phase of evolution. It is two rotation periods before that of the 170 ± 20 km/s jet in the third panel. This may account for increase of intensity of the outer knots as they are closer to the leading bow shock. However, it shows a high amplitude of velocity perturbation cannot increase the intensity of emission near the source in our model.
A study of the wiggle morphology of HH 211 through numerical simulations
Three extremely young low-mass protostars, B1-bN, B1-bS, and B1-c, observed with the ALMA at a resolution of ~0.2" (= 47 au). The upper panels show the images of C17O 2-1 emission, the lower panels show the methanol images (color) overlaid on the 1.3 mm continuum images (white contours).
ALMA revealed the earliest stage of protostellar evolution
An extremely young protostar, SMM11, in the Serpens Main cluster forming region observed with ALMA in 1.3 mm continuum, 12CO J=2-1 line, and C18O J=2-1 line. These results, as well as submillimeter and infrared results, suggest that the protostar is in an early phase of star formation right after the second collapse.
An extremely young protostar, SMM11, observed in millimeter wavelength
Visibility distribution of the protostar L1527 IRS observed with ALMA in 220 GHz continuum. Visibility distributions are the Fourier transform of images. The amplitude distribution of this protostar is narrower in the north-south direction (red) than in the east-west direction (blue), revealing 2D structures even in the Fourier domain.
Visibility distribution of the protostar L1527 IRS in 220 GHz continuum
The image shows the turbulent gas when a supernova collides with a nearby star-forming galaxy.
How a supernova affects a nearby star-forming galaxy?
<b>Left:</b> near infrared [Fe II] 1.644 µm + continuum image of the wide binary FS Tau A and B. FS Tau B is not visible but its adjacent reflection nebula R3 is bright in continuum. Jet and counterjet driven from FS Tau B along 55 degrees are indicated. <br> <b>Right:</b> continuum-subtracted position-velocity diagram of FS Tau B jet in [Fe II] along the position angle of the jet. The position of the invisible driving source is indicated by the horizontal dashed line and the systemic velocity is labeled by the vertical dash-dotted line. The blueshifted and redshifted knots have velocities -74.6 and +55.8 km/s, respectively.
Is FS Tau B Driving an Asymmetric Jet?
<b>Left:</b> near infrared [Fe II] 1.644 µm + continuum image of the wide binary FS Tau A and B. FS Tau B is not visible but its adjacent reflection nebula R3 is bright in continuum. Jet and counterjet driven from FS Tau B along 55 degrees are indicated. <br> <b>Right:</b> continuum-subtracted position-velocity diagram of FS Tau B jet in [Fe II] along the position angle of the jet. The position of the invisible driving source is indicated by the horizontal dashed line and the systemic velocity is labeled by the vertical dash-dotted line. The blueshifted and redshifted knots have velocities -74.6 and +55.8 km/s, respectively.
Is FS Tau B Driving an Asymmetric Jet?
<b>Left:</b> near infrared [Fe II] 1.644 µm + continuum image of the wide binary FS Tau A and B. FS Tau B is not visible but its adjacent reflection nebula R3 is bright in continuum. Jet and counterjet driven from FS Tau B along 55 degrees are indicated. <br> <b>Right:</b> continuum-subtracted position-velocity diagram of FS Tau B jet in [Fe II] along the position angle of the jet. The position of the invisible driving source is indicated by the horizontal dashed line and the systemic velocity is labeled by the vertical dash-dotted line. The blueshifted and redshifted knots have velocities -74.6 and +55.8 km/s, respectively.
Is FS Tau B Driving an Asymmetric Jet?
<b>(a)</b> Position–velocity (PV) diagram of the [Ne III] λ3869 line from Sz 102, after Gaussian decomposition. The emission corresponds to the blueshifted and redshifted microjets is shown in blue and red contours, respectively. The spectra have been binned every 10 km s<sup>−1</sup> and smoothed with Gaussian with σ<sub>G</sub> = 1.0 pixel. <br> <b>(b)</b> Decomposed [Ne III] λ3869 line profiles normalized to the redshifted peak intensity. The blueshifted and redshifted emissions are shown as blue and red histograms, respectively. For each decomposed line profile, a single Gaussian is fitted and is shown as blue and red thick lines, respectively.
Velocity-Resolved [Ne III] from X-ray Irradiated Sz 102 Microjets
<b>(a)</b> Position–velocity (PV) diagram of the [Ne III] λ3869 line from Sz 102, after Gaussian decomposition. The emission corresponds to the blueshifted and redshifted microjets is shown in blue and red contours, respectively. The spectra have been binned every 10 km s<sup>−1</sup> and smoothed with Gaussian with σ<sub>G</sub> = 1.0 pixel. <br> <b>(b)</b> Decomposed [Ne III] λ3869 line profiles normalized to the redshifted peak intensity. The blueshifted and redshifted emissions are shown as blue and red histograms, respectively. For each decomposed line profile, a single Gaussian is fitted and is shown as blue and red thick lines, respectively.
Velocity-Resolved [Ne III] from X-ray Irradiated Sz 102 Microjets
0.9-mm dust-continuum image of the protostellar binary L1551 NE observed with ALMA (left), and that predicted from our supercomputer numerical simulation (right). Green curves in the left panel traces the observed structures of the circumbinary spirals (Takakuwa et al. 2014, ApJ, 796, 1).
ALMA Observation of Gas Spirals as a Nursery of Binary Stars
Dust distribution in the binary protostellar system L1551 NE observed with the SMA in 0.9 mm continuum. Crosses show the position of each binary component. Dashed curves delineate the ring-like “circumbinary disk” components. (Takakuwa et al. 2012, ApJ, 754, 52)
Dust distribution in the binary protostellar system L1551 NE observed with the SMA in 0.9 mm continuum.
(a) Schematic figure of our kinematic model. Red and blue arrows denote the directions of the outflow from the protostar. This protostar is surrounded by a Keplerian disk, and there two streams of infalling flow connecting the disk. The infalling flows transfer mass and angular momentum to the disk, allowing it to grow. (b) Image of the observed gas distribution around the protostar (contour) overlaid on the model distribution generated using our kinematic model (color). A cross shows the location of the protostar.
Infalling Flow toward a Keplerian Disk around the Protostar L1489 IRS
SMA images of the C18O (2-1) emission in the 17 Class 0 and 0/I protostellar sources. Contours show the intensity distribution of the C18O (2-1) emission, tracing the distribution of the gas around the protostars. Color scales show the mean velocity of the C18O (2-1) emission, tracing the motions of the ambient gas. Blue and red arrows denote the directions of the outflowing gas associated with these protostar, which can represent the rotational axes of these systems. Black arrows on the tops of filled white circle show the directions that how the mean velocities change with the positions. If the directions of the trends in the changes of the motional velocities are more perpendicular to the rotational axes, the sources likely exhibit faster rotational motions dominant over infalling velocities, and hence larger circumstellar disks.
Infalling and Rotational Motions of Ambient Gas around 17 Protostars
This artist's concept shows a still-forming protostar which is accreting material from a surrounding disk. Some of the material from the disk, rather than falling onto the star, is ejected outward in a bipolar jet. New measurements from the Submillimeter
A still-forming protostar which is accreting material from a surrounding disk
This artist's concept shows a still-forming protostar which is accreting material from a surrounding disk. Some of the material from the disk, rather than falling onto the star, is ejected outward in a bipolar jet. New measurements from the Submillimeter
A still-forming protostar which is accreting material from a surrounding disk
Two submm sources in the B1-b molecular cloud core. (Left) Thermal dust emission at 1.1 mm observed with the SMA (white contours) on top of the mid-IR image taken with the Spitzer space telescope (color image). (Right) N2D+ emission line observed with the SMA and SMT. (Huang & Hirano 2013, ApJ, 766, 131)
Two submm sources in the B1-b molecular cloud core.

恆星由分子雲形成，為宇宙最基本的組成份子。恆星形成的過程改變了分子雲的物理及化學環境，因此不僅控制了星系的結構和演化，也掌控了重元素逐步生成，及讓生命得以產生的行星環境。在如此的動力過程中，分子雲收縮產生了分子雲核，進而因重力坍縮形成年輕星體,接下來經由拱星盤發生物質吸積，這又伴隨著如恆星風，噴流或外向流導致物質流失，最終分子雲包層潰散。這只是我們所了解恆星形成的約略過程，但其細節尙未完全了解，故仍為現代天文學中的主要研究課題。本所恆星形成研究小組致力於以理論模型及觀測上的證據來了解恆形形成過程的本質。

研究人員 (26)

李景輝 Lee, Chin-Fei cv 副所長; 特聘研究員
研究興趣: 恆星形成及演化; 電波觀測及流體動力數值模擬
平野尚美 Hirano, Naomi cv 研究員
研究興趣: 電波天文學，恆星形成及星際介質
高培邁 Koch, Patrick cv 研究員
研究興趣: 觀測宇宙學, 星系團
呂聖元 Liu, Sheng-Yuan cv 研究員
研究興趣: 恆星形成，天文化學
大橋永芳 Ohashi, Nagayoshi cv 研究員
研究興趣: 恆星及行星形成，分子雲，干涉儀
尚賢 Shang, Hsien cv 研究員
研究興趣: 理論及計算天文物理，恆星及行星形成，磁流體動力學，噴流，隕石
高見道弘 Takami, Michihiro cv 副研究員長聘
研究興趣: 恆星形成,光學/紅外線光譜學
顏士韋 Yen, Hsi-Wei cv 副研究員長聘
研究興趣: 電波天文學, 恆星形成, 原行星盤
陳科榮 Chen, Ke-Jung cv 助研究員
研究興趣: 理論與計算天文物理: 大質量恆與超新星爆炸, 星際介質, 超大質量黑洞, 第一代恆星與星系
湯雅雯 Tang, Ya-Wen cv 助研究員
研究興趣: 恆星形成; 磁場觀測; 原恆星形成盤面
賀曾樸 Ho, Paul cv 通信研究員
研究興趣: 電波天文學
管一政 Kuan, Yi-Jehng cv 研究員; 師大地科系合聘
研究興趣: 天文化學，分子天文物理，分子雲及天文生物學
林仁良 Lim, Jeremy cv 兼任研究員; 香港大學
研究興趣: 電波天文學, 恆星形成及演化, 星系
賴詩萍 Lai, Shih-Ping cv 訪問學者 (清華大學物理系)
研究興趣: 天文物理(實驗), 恆星形成
李昫岱 Lee, Hsu-Tai cv 訪問學者
研究興趣: 恆星形成
潘保玉 Phan, Bao-Ngoc cv 訪問學者 (越南胡志明國際大學物理系)
研究興趣: 極低質量恆星
高橋智子 Takahashi, Satoko cv 訪問學者 (日本國家天文台)
研究興趣: 恆星形成; 電波天文學
高桑繁久 Takakuwa, Shigehisa cv 訪問學者 (鹿兒島大學)
研究興趣: 恆星形成, 次毫米波天文學及干涉儀
蘇裕農 Su, Yu-Nung cv 計畫研究經理/ALMA ARC 經理
研究興趣: 恆星形成，電波天文學
卡兒 Karr, Jennifer cv 支援科學家
研究興趣: 恆星形成; 星際介質
劉君帆 Liu, Chun-Fan cv Theory 支援科學家
研究興趣: 恆星形成；可見光與紅外光天文學；科學運算程式開發
韋米卡 Vaisala, Miikka cv 計畫科學家
研究興趣: 磁流力湍流與恆星形成
顏吉鴻 Yan, Chi-Hung cv OIR/EPO計畫支援工程師
研究興趣: 紅外線影像處理, 電波天文學
柯理思 Flores Gonzalez, Christian Alejandro cv 博士後研究
研究興趣: 恆星形成
陸哲軒 Thieme, Travis John cv 博士後研究
研究興趣: 恆星形成、原恆星盤形成與演化、電波天文學
山口正行 Yamaguchi, Masayuki cv 博士後研究
研究興趣: 行星形成；環星盤結構及其演化。電波天文學；無線電干涉儀的孔徑合成和成像技術。統計數學（稀疏建模）和機器學習。

期刊論文 (477)

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  3. Motoyama K; Krasnopolsky R; Shang H; Aida K; Sakane E, "An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices" , ApJS: 270(2), id.19 (11 pp), Jan, 2024 [SCI] ( ADS | Fulltext )
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  11. Gu P-G; Chen C-Y; Shen E; Yen C-C, Lin MK, "Revealing the Drag Instability in One-fluid Nonideal Magnetohydrodynamic Simulations of a 1D Isothermal C-shock" , ApJ: 935(2), id.95 (16pp), Aug, 2022 [SCI] ( ADS | Fulltext )
  12. Gupta A; Yen H-W; Koch P; Bastien P; Bourke TL; Chung EJ; Hasegawa T; Hull CLH; Inutsuka S-I; Kwon J; Kwon W; Lai S-P; Lee CW; Lee C-F; Pattle K; Qiu K; Tahani M; Tamura M; Ward-Thompson D, "Effects of magnetic field orientations in dense cores on gas kinematics in protostellar envelopes" , ApJ: 930(1), id.67 (17pp), May, 2022 [SCI] ( ADS | Fulltext )
  13. Hsu S-Y; Liu S-Y; Liu T; Sahu D; Lee C-F; Tatematsu K; Kim K-T; Hirano N; Yang Y-L; Johnstone D; Liu H; Juvela M; Bronfman L; Chen H-RV; Dutta S; Eden DJ; Jhan K-S; Kuan Y-J; Lee CW; Lee J-E; Li S; Liu C-F; Qin S-L; Sanhueza P; Shang H; Soam A; Traficante A; Zhou J, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): A Hot Corino Survey toward Protostellar Cores in the Orion Cloud" , ApJ: 927(2), id.218 (27pp), March, 2022 [SCI] ( ADS | Fulltext )
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  16. Wang W; Väisälä MS; Shang H; Krasnopolsky R; Li Z-Y; Lam KH; Yuan F, "Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Fields" , ApJ: 928(1), id.85 (23pp), March, 2022 [SCI] ( ADS | Fulltext )
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