Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
Star formation is ubiquitously associated with the ejection of accretion-powered outflows that carve bipolar cavities through the infalling envelope. This feedback is expected to be important for regulating the efficiency of star formation from a natal prestellar core. These low-extinction outflow c...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acbd47 |
| _version_ | 1797701919558336512 |
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| author | Jan E. Staff Kei E. I. Tanaka Jon P. Ramsey Yichen Zhang Jonathan C. Tan |
| author_facet | Jan E. Staff Kei E. I. Tanaka Jon P. Ramsey Yichen Zhang Jonathan C. Tan |
| author_sort | Jan E. Staff |
| collection | DOAJ |
| description | Star formation is ubiquitously associated with the ejection of accretion-powered outflows that carve bipolar cavities through the infalling envelope. This feedback is expected to be important for regulating the efficiency of star formation from a natal prestellar core. These low-extinction outflow cavities greatly affect the appearance of a protostar by allowing the escape of shorter-wavelength photons. Doppler-shifted CO line emission from outflows is also often the most prominent manifestation of deeply embedded early-stage star formation. Here, we present 3D magnetohydrodynamic simulations of a disk wind outflow from a protostar forming from an initially 60 M _⊙ core embedded in a high-pressure environment typical of massive star-forming regions. We simulate the growth of the protostar from m _* = 1 M _⊙ to 26 M _⊙ over a period of ∼100,000 yr. The outflow quickly excavates a cavity with a half opening angle of ∼10° through the core. This angle remains relatively constant until the star reaches 4 M _⊙ . It then grows steadily in time, reaching a value of ∼50° by the end of the simulation. We estimate a lower limit to the star formation efficiency (SFE) of 0.43. However, accounting for continued accretion from a massive disk and residual infall envelope, we estimate that the final SFE may be as high as ∼0.7. We examine observable properties of the outflow, especially the evolution of the cavity's opening angle, total mass, and momentum flux, and the velocity distributions of the outflowing gas, and compare with the massive protostars G35.20-0.74N and G339.88-1.26 observed by the Atacama Large Millimeter/submillimeter Array (ALMA), yielding constraints on their intrinsic properties. |
| first_indexed | 2024-03-12T04:42:35Z |
| format | Article |
| id | doaj.art-13ff581f34794773b7df8d6035178747 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:42:35Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-13ff581f34794773b7df8d60351787472023-09-03T09:30:42ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194714010.3847/1538-4357/acbd47Disk Wind Feedback from High-mass Protostars. II. The Evolutionary SequenceJan E. Staff0https://orcid.org/0000-0001-9040-8525Kei E. I. Tanaka1https://orcid.org/0000-0002-6907-0926Jon P. Ramsey2https://orcid.org/0000-0002-3835-3990Yichen Zhang3https://orcid.org/0000-0001-7511-0034Jonathan C. Tan4https://orcid.org/0000-0002-3389-9142Department of Space, Earth & Environment, Chalmers University of Technology , Gothenburg, Sweden ; jestaff.astro@gmail.com; College of Science and Math, University of the Virgin Islands , St Thomas, 00802, Virgin Islands, USADepartment of Earth and Planetary Sciences, Tokyo Institute of Technology , Meguro, Tokyo, 152-8551, Japan; Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado Boulder , Boulder, CO 80309, USA; ALMA Project, National Astronomical Observatory of Japan , Mitaka, Tokyo 181-8588, JapanDepartment of Astronomy, University of Virginia , Charlottesville, VA 22904, USADepartment of Astronomy, University of Virginia , Charlottesville, VA 22904, USADepartment of Space, Earth & Environment, Chalmers University of Technology , Gothenburg, Sweden ; jestaff.astro@gmail.com; Department of Astronomy, University of Virginia , Charlottesville, VA 22904, USAStar formation is ubiquitously associated with the ejection of accretion-powered outflows that carve bipolar cavities through the infalling envelope. This feedback is expected to be important for regulating the efficiency of star formation from a natal prestellar core. These low-extinction outflow cavities greatly affect the appearance of a protostar by allowing the escape of shorter-wavelength photons. Doppler-shifted CO line emission from outflows is also often the most prominent manifestation of deeply embedded early-stage star formation. Here, we present 3D magnetohydrodynamic simulations of a disk wind outflow from a protostar forming from an initially 60 M _⊙ core embedded in a high-pressure environment typical of massive star-forming regions. We simulate the growth of the protostar from m _* = 1 M _⊙ to 26 M _⊙ over a period of ∼100,000 yr. The outflow quickly excavates a cavity with a half opening angle of ∼10° through the core. This angle remains relatively constant until the star reaches 4 M _⊙ . It then grows steadily in time, reaching a value of ∼50° by the end of the simulation. We estimate a lower limit to the star formation efficiency (SFE) of 0.43. However, accounting for continued accretion from a massive disk and residual infall envelope, we estimate that the final SFE may be as high as ∼0.7. We examine observable properties of the outflow, especially the evolution of the cavity's opening angle, total mass, and momentum flux, and the velocity distributions of the outflowing gas, and compare with the massive protostars G35.20-0.74N and G339.88-1.26 observed by the Atacama Large Millimeter/submillimeter Array (ALMA), yielding constraints on their intrinsic properties.https://doi.org/10.3847/1538-4357/acbd47Star formationStellar windsMassive stars |
| spellingShingle | Jan E. Staff Kei E. I. Tanaka Jon P. Ramsey Yichen Zhang Jonathan C. Tan Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence The Astrophysical Journal Star formation Stellar winds Massive stars |
| title | Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence |
| title_full | Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence |
| title_fullStr | Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence |
| title_full_unstemmed | Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence |
| title_short | Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence |
| title_sort | disk wind feedback from high mass protostars ii the evolutionary sequence |
| topic | Star formation Stellar winds Massive stars |
| url | https://doi.org/10.3847/1538-4357/acbd47 |
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