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...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Jan E. Staff [verfasserIn] Kei E. I. Tanaka [verfasserIn] Jon P. Ramsey [verfasserIn] Yichen Zhang [verfasserIn] Jonathan C. Tan [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Star formation Stellar winds Massive stars

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 947(2023), 1, p 40
Übergeordnetes Werk:	volume:947 ; year:2023 ; number:1, p 40

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/acbd47

Katalog-ID:	DOAJ089151909

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allfields	10.3847/1538-4357/acbd47 doi (DE-627)DOAJ089151909 (DE-599)DOAJ13ff581f34794773b7df8d6035178747 DE-627 ger DE-627 rakwb eng QB460-466 Jan E. Staff verfasserin aut Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Star formation Stellar winds Massive stars Astrophysics Kei E. I. Tanaka verfasserin aut Jon P. Ramsey verfasserin aut Yichen Zhang verfasserin aut Jonathan C. Tan verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 947(2023), 1, p 40 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:947 year:2023 number:1, p 40 https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/article/13ff581f34794773b7df8d6035178747 kostenfrei https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 947 2023 1, p 40
spelling	10.3847/1538-4357/acbd47 doi (DE-627)DOAJ089151909 (DE-599)DOAJ13ff581f34794773b7df8d6035178747 DE-627 ger DE-627 rakwb eng QB460-466 Jan E. Staff verfasserin aut Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Star formation Stellar winds Massive stars Astrophysics Kei E. I. Tanaka verfasserin aut Jon P. Ramsey verfasserin aut Yichen Zhang verfasserin aut Jonathan C. Tan verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 947(2023), 1, p 40 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:947 year:2023 number:1, p 40 https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/article/13ff581f34794773b7df8d6035178747 kostenfrei https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 947 2023 1, p 40
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allfieldsGer	10.3847/1538-4357/acbd47 doi (DE-627)DOAJ089151909 (DE-599)DOAJ13ff581f34794773b7df8d6035178747 DE-627 ger DE-627 rakwb eng QB460-466 Jan E. Staff verfasserin aut Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Star formation Stellar winds Massive stars Astrophysics Kei E. I. Tanaka verfasserin aut Jon P. Ramsey verfasserin aut Yichen Zhang verfasserin aut Jonathan C. Tan verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 947(2023), 1, p 40 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:947 year:2023 number:1, p 40 https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/article/13ff581f34794773b7df8d6035178747 kostenfrei https://doi.org/10.3847/1538-4357/acbd47 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 947 2023 1, p 40
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author	Jan E. Staff
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title	Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
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title_sort	disk wind feedback from high-mass protostars. ii. the evolutionary sequence
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title_auth	Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
abstract	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.
abstractGer	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.
abstract_unstemmed	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.
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title_short	Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
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Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence

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