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Figure shows an example of a nested-grid mesh refinement (NMR) run carried out by the Antares code for a global protoplanetary disk with an embedded circumplanetary disk surrounding a 0.05-Jupiter-mass planet at 5.2 AU from the star at origin. The simulation has 6 levels of refinement, with the finest resolution of 6.25×10–4 AU, resolving the Hill radius of the planet (0.13 AU at 5.2 AU) with ~200 cells. (Antares code with the CompAS project)
Formation and Evolution of Protoplanetary and Circumplanetary Disks with Antares Three-Dimensional Global Hydrodynamic Simulations
Left – Surface density distribution of a forming circumplanetary disk in a protoplanetary disk with the Antares three-dimensional global simulation. A planet of one-Jupiter mass is placed at (x,y) = (5.2,0) au. The color scale is stretched logarithmically. The level boundaries of the nested-grid mesh refinement are shown in white lines. Center – Temperature distribution of the disk obtained with the radiative transfer code Hyperion. The photon sources are the central 4500-K star and an accreting planet of ~1000 K at 5.2 au from the star. The circumplanetary dust is heated up to ~ 1000 K and produces thermal emission. Right – Monochromatic synthetic image corresponding to the 1-mm dust continuum imaging, obtained with Hyperion. The surface brightness is logarithmically stretched in units of MJy/arcsec2.
Dust Radiative Transfer on a Global Hydrodynamic Simulation of a Forming Circumplanetary Disk
<b>Left</b> – Surface density distribution of a forming circumplanetary disk in a protoplanetary disk with the Antares three-dimensional global simulation. A planet of one-Jupiter mass is placed at (x,y) = (5.2,0) au. The color scale is stretched logarithmically. The level boundaries of the nested-grid mesh refinement are shown in white lines. <b>Center</b> – Temperature distribution of the disk obtained with the radiative transfer code Hyperion. The photon sources are the central 4500-K star and an accreting planet of ~1000 K at 5.2 au from the star. The circumplanetary dust is heated up to ~ 1000 K and produces thermal emission. <b>Right</b> – Monochromatic synthetic image corresponding to the 1-mm dust continuum imaging, obtained with Hyperion. The surface brightness is logarithmically stretched in units of MJy/arcsec<sup>2</sup>.
Dust Radiative Transfer on a Global Hydrodynamic Simulation of a Forming Circumplanetary Disk
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
Figure: Example of a nested-grid mesh refinement (NMR) run of a global protoplanetary disk with an embedded circumplanetary disk surrounding a 0.05-Jupiter-mass planet at 5.2 AU from the star at origin. The simulation has 6 levels of refinement, with the finest resolution of 6.25×10–4 AU, resolving the Hill radius of the planet (0.13 AU at 5.2 AU) with ~200 cells.
Formation and Evolution of Protoplanetary and Circumplanetary Disks with Antares Three-Dimensional Global Hydrodynamic Simulations
<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?
Figure (a) shows the normalized line profiles of the Ne II 12.81um (blue), Ne III 15.55um (red), and the O I 6300 (black) lines for a X-Wind jet modeled for a typical T Tauri star, at an inclination angle of 45 degrees. Figure (b) shows the contribution of the Ne II line as a function of cylindrical distance to the jet axis.
Neon Fine-Structure Line Emission from the Outflows of Young Stellar Objects
<b>Left:</b> position-velocity diagrams of RW Aur A redshifted and blueshifted jets in [S II] emission line are shown in the upper two panels. Observed (black) and synthetic (red and blue for the redshifted and blueshifted jets, respectively) spectra are compared. Velocity centroids fitted from the observed (discrete symbols) and synthetic (thick lines) line spectra are shown in the lower panel. <br> <b>Right:</b> Cross line-ratio plots obtained from observed (discrete symbols) and synthetic (shaded areas) spectra. The difference in physical conditions of the jets and the match between observations and models can be seen.
RW Aur A from the X-Wind Point of View: General Features
<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
The figure shows the density structures at 100 (top) and 1000 (bottom) years with four representative numbers n = 1, 2, 4, 6 (from left to right), which indicates the degree of anisotropy in ambient mass distribution.
Unified Model for Jets and Outflows from Young Stars
Liu, Chun-Fan
Theory Support Scientist
photo of Liu, Chun-Fan
Office: ASMAB 1201
TEL: +886-2-2366-5382
FAX: +886-2-2367-7849
Email: cfliu_replace2@_asiaa.sinica.edu.tw

Education and Positions

  • TIARA Junior Support Scientist, Institute of Astronomy and Astrophysics, Academia Sinica (2015~present)
  • Ph.D., Graduate Institute of Astrophysics, National Taiwan University (2008~2015)

Research Interests

Optical/Infrared diagnostics of jets from T Tauri stars, Radiative transfer simulations of line and continuum emission from protostellar jets and disks

Journal Papers affiliated with ASIAA

  1. Ai T-H; Liu C-F; Shang H; Johnstone D; Krasnopolsky R, "A Unified Model for Bipolar Outflows from Young Stars: Kinematic and Mixing Structures in HH 30" , ApJ: 964(2), id.147 (15 pp), Apr, 2024 [SCI] ( ADS | Fulltext )
  2. Hsu S-Y; Liu S-Y; Johnstone D; Liu T; Bronfman L; Chen H-RV; Dutta S; Eden DJ; Evans NJ, Ii; Hirano N; Juvela M; Kuan Y-J; Kwon W; Lee C-F; Lee CW; Lee J-E; Li S; Liu C-F; Liu X; Luo Q; Qin S-L; Rawlings MG; Sahu D; Sanhueza P; Shang H; Tatematsu K; Yang Y-L, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-Envelope Origin of Hot Corinos" , ApJ: 956(2), id.120 (23pp), Oct, 2023 [SCI] ( ADS | Fulltext )
  3. Kiefer F; Hébrard G; Martioli E; Artigau E; Doyon R; Donati J-F; Cadieux C; Carmona A; Ciardi DR; Cristofari PI; de Almeida L; Figueira P; Gaidos E; Gonzales E; Lecavelier Des Etangs A; Stassun KG; Arnold L; Benneke B; Boisse I; Bonfils X; Cook NJ; Cortés-Zuleta P; Delfosse X; do Nascimento JD; Fausnaugh M; Fong W; Fouqué P; Forveille T; Gomes da Silva J; Hesse K; Kóspál Á; Lewis H; Liu C-F; Martins JHC; Paegert M; Seager S; Shang H; Twicken JD; Vandal T; Vinatier S; Widemann T; Winn JN, "A sub-Neptune planet around TOI-1695 discovered and characterized with SPIRou and TESS" , A&A: 670, id.A136 (28 pp), Feb, 2023 [SCI] ( ADS | Fulltext )
  4. Shang H; Krasnopolsky R; Liu C-F, "A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration" , ApJL: 945(1), id.L1 (21 pp), March, 2023 [SCI] ( ADS | Fulltext )
  5. Shang H; Liu C-F; Krasnopolsky R; Wang L-Y, "A Unified Model for Bipolar Outflows from Young Stars: Kinematic Signatures of Jets, Winds, and Their Magnetic Interplay with the Ambient Toroids" , ApJ: 944(2), id.230 (55 pp), Feb, 2023 [SCI] ( ADS | Fulltext )
  6. Takami M; Guenther HM; Schneider PC; Beck TL; Karr JL; Ohyama Y; Galvan-Madrid R; Uyama T; White M; Grankin K; Coffey D; Liu C-F; Fukagawa M; Manset N; Chen W-P; Pyo T-S; Shang H; Ray TP; Otsuka M; Chou M-Y, "Time-variable Jet Ejections from RW Aur A, RY Tau, and DG Tau" , ApJS: 264(1), id.1 (19pp), Jan, 2023 [SCI] ( ADS | Fulltext )
  7. Dutta S; Lee C-F; Johnstone D; Liu T; Hirano N; Liu S-Y; Lee J-E; Shang H; Tatematsu KI; Kim K-T; Sahu D; Sanhueza P; Di Francesco J; Jhan K-S; Lee CW; Kwon W; Li S; Bronfman L; Liu H-L; Traficante A; Kuan Y-J; Hsu S-Y; Moraghan A; Liu C-F; Eden D; Soam A; Luo Q; ALMASOP Team, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Detection of a Dense SiO Jet in the Evolved Protostellar Phase" , ApJ: 925(1), id.11 (10pp), Jan, 2022 [SCI] ( ADS | Fulltext )
  8. 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 )
  9. Jhan K-S; Lee C-F; Johnstone D; Liu T; Liu S-Y; Hirano N; Tatematsu KI; Dutta S; Moraghan A; Shang H; Lee J-E; Li S; Liu C-F; Hsu S-Y; Kwon W; Sahu D; Liu X-C; Kim K-T; Luo Q; Qin S-L; Sanhueza P; Bronfman L; Qizhou Z; Eden D; Traficante A; Lee CW; Almasop T, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from Their SiO Knots" , ApJL: 931(1), id.L5 (9pp), May, 2022 [SCI] ( ADS | Fulltext )
  10. Liu C-F; Shang H; Herczeg GJ; Walter FM, "Revealing Ionization Conditions of Sz 102 with Spatially Resolved [Ne III] Microjets" , ApJ: 909(2), id.196 (12pp), Mar, 2021 [SCI] ( ADS | Fulltext )
  11. Shang H; Krasnopolsky R; Liu C-F; Wang L-Y, "A Unified Model for Bipolar Outflows from Young Stars: The Interplay of Magnetized Wide-angle Winds and Isothermal Toroids" , ApJ: 905(2), id.116 (52pp.), Dec, 2020 [SCI] ( ADS | Fulltext )
  12. Takami M; ...; Karr JL; Ohyama Y; ...; Liu HB; ...; Liu CF; ...; Shang H; ...; Chou MY, "Possible Time Correlation between Jet Ejection and Mass Accretion for RW Aur A" , ApJ: 901(1), id.24 (9pp.), Sep, 2020 [SCI] ( ADS | Fulltext )
  13. Gully-Santiago MA; Herczeg GJ; Czekala I; ...; Liu C-F, "Placing the spotted T Tauri star LkCa 4 on an HR diagram" , ApJ: 836(2), 200, Feb, 2017 [SCI] ( ADS | Fulltext )
  14. Liu C-F; Shang H; Herczeg GJ; Walter FM, "The [Ne III] Jet of DG Tau and Its Ionization Scenarios" , ApJ: 832(2), 153, Dec, 2016 [SCI] ( ADS | Fulltext )
  15. Liu C-F; Shang H; Walter FM; Herczeg GJ, "Velocity-resolved [Ne III] from X-Ray Irradiated Sz 102 Microjets" , ApJ: 786(2), 99, May, 2014 [SCI] ( ADS | Fulltext )
  16. Liu C-F; Shang H, "RW Aur A from the X-Wind Point of View: General Features" , ApJ: 761(2), 94, Dec, 2012 [SCI] ( ADS | Fulltext )
  17. Liu C-F; Shang H; Pyo T-S; Takami M; ...; Yan C-H; Wang SY; Ohashi N; Hayashi M, "Is FS Tau B Driving an Asymmetric Jet?" , ApJ: 749(1), 62, April 10, 2012 [SCI] ( ADS | Fulltext )
  18. Shang H; Glassgold AE; Lin W-C; Liu C-F, "Ne II Fine-structure Line Emission from the Outflows of Young Stellar Objects" , ApJ: 714(2), 1733-1739, May, 2010 [SCI] ( ADS | Fulltext )
  19. Shang H; Allen A; Li Z-Y; Liu C-F; Chou M-Y; Anderson J, "A Unified Model for Bipolar Outflows from Young Stars" , ApJ: 649(2), 845-855, Oct, 2006 [SCI] ( ADS | Fulltext )
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