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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
Moraghan, Anthony
ALMA Support Scientist and ACDC Deputy Manager
photo of Moraghan, Anthony
Office: ASMAB 1404
TEL: +886-2-2366-5461
FAX: +886-2-2367-7849
Email: ajm_replace2@_asiaa.sinica.edu.tw

Research Interests

Star formation; Numerical simulations of jets and outflows

Journal Papers affiliated with ASIAA

  1. Lee C-F; Jhan K-S; Moraghan A, "First Detection of a Linear Structure in the Midplane of the Young HH 211 Protostellar Disk: A Spiral Arm?" , ApJL: 951(1), id.L2 (8pp), July, 2023 [SCI] ( ADS | Fulltext )
  2. Prokhorov DA; Moraghan A, "An update on Fermi-LAT transients in the Galactic plane, including strong activity of Cygnus X-3 in mid-2020" , MNRAS: 519(2), 2680-2689, Feb, 2023 [SCI] ( ADS | Fulltext )
  3. Dutta S; Lee C-F; Hirano N; Liu T; Johnstone D; Liu S-Y; Tatematsu K; Goldsmith PF; Sahu D; Evans NJ; Sanhueza P; Kwon W; Qin S-L; Ranjan Samal M; Zhang Q; Kim K-T; Shang H; Lee CW; Moraghan A; Jhan K-S; Li S; Lee J-E; Traficante A; Juvela M; Bronfman L; Eden D; Soam A; He J; Liu H-L; Kuan Y-J; Pelkonen V-M; Luo Q; Yi H-W; Hsu S-Y, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar evolution" , ApJ: 931(2), id.130 (13pp), June, 2022 [SCI] ( ADS | Fulltext )
  4. 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 )
  5. 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 )
  6. Prokhorov DA; Moraghan A; Vink J, "Search for gamma rays from SNe with a variable-size sliding-time-window analysis of the Fermi-LAT data" , MNRAS: 505(1), 1413–1421, Jul, 2021 [SCI] ( ADS | Fulltext )
  7. Sahu D; Liu S-Y; Liu T; Evans NJ, Ii; Hirano N; Tatematsu KI; Lee C-F; Kim K-T; Dutta S; Alina D; Bronfman L; Cunningham M; Eden DJ; Garay G; Goldsmith PF; He J; Hsu S-Y; Jhan K-S; Johnstone D; Juvela M; Kim G; Kuan Y-J; Kwon W; Lee CW; Lee J-E; Li D; Li PS; Li S; Luo Q-Y; Montillaud J; Moraghan A; Pelkonen V-M; Qin S-L; Ristorcelli I; Sanhueza P; Shang H; Shen Z-Q; Soam A; Wu Y; Zhang Q; Zhou J, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Detection of Extremely High-density Compact Structure of Prestellar Cores and Multiple Substructures Within" , ApJL: 907(1), L15 (9pp), Jan, 2021 [SCI] ( ADS | Fulltext )
  8. Dutta S; Lee CF; Liu T; Hirano N; Liu SY; ... ; Shang H; Sahu D;...; Moraghan A; Jhan KS; Hsu SY;...; Kuan YJ; et al., "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP). II. Survey Overview: A First Look at 1.3 mm Continuum Maps and Molecular Outflows" , ApJS: 251(2), id.20 (35pp.), Dec, 2020 [SCI] ( ADS | Fulltext )
  9. Hsu SY; Liu SY; ...; Sahu D; Hirano N; Lee CF; ...; Dutta S; ...; Jhan K-S; ...; Kuan YJ; ...; Moraghan A; ...; Shang H, "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP). I. Detection of New Hot Corinos with the ACA" , ApJ: 898(2), id.107 (37pp.), Aug, 2020 [SCI] ( ADS | Fulltext )
  10. Prokhorov DA; Moraghan A, "A geomagnetic filter for the Fermi-LAT background" , MNRAS: 490(4), 5440-5450, Dec, 2019 [SCI] ( ADS | Fulltext )
  11. Prokhorov DA; Moraghan A, "A search for cyclical sources of γ-ray emission on the period range from days to years in the Fermi-LAT sky" , MNRAS: 471(3), 3036-3042, Nov, 2017 [SCI] ( ADS | Fulltext )
  12. Huang P-S; Lee C-F; Moraghan A; Smith M, "The Shaping of the Multipolar Pre-planetary Nebula CRL 618 by Multidirectional Bullets" , ApJ: 820(2), 134, April, 2016 [SCI] ( ADS | Fulltext )
  13. Moraghan A; Lee C-F; Huang P-S; Vaidya, Bhargav, "A study of the wiggle morphology of HH 211 through numerical simulations" , MNRAS: 460(2), 1829-1838, Aug 1, 2016 [SCI] ( ADS | Fulltext )
  14. Prokhorov D; Moraghan A, "A search for pair haloes around active galactic nuclei through a temporal analysis of Fermi-Large Area Telescope data" , MNRAS: 457(3), 2433-2444, April 11, 2016 [SCI] ( ADS | Fulltext )
  15. Moraghan A; Kim J; Yoon S-J, "Power spectra of outflow-driven turbulence" , MNRAS: 450(1), 360-368, June, 2015 [SCI] ( ADS | Fulltext )
  16. Pasquato M; de Luca A; Raimondo G; Carini R; Moraghan A; et al., "Stellar Encounter Driven Red-giant Star Mass Loss in Globular Clusters" , ApJ: 789(1), 28, July, 2014 [SCI] ( ADS | Fulltext )
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