Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow

We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by th...
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Autor*in:	J. A. López-Vázquez [verfasserIn] Chin-Fei Lee [verfasserIn] M. Fernández-López [verfasserIn] Fabien Louvet [verfasserIn] O. Guerra-Alvarado [verfasserIn] Luis A. Zapata [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 962(2024), 1, p 28
Übergeordnetes Werk:	volume:962 ; year:2024 ; number:1, p 28

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad132a

Katalog-ID:	DOAJ09595998X

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520			\|a We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind.
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allfields	10.3847/1538-4357/ad132a doi (DE-627)DOAJ09595998X (DE-599)DOAJacdf9ab14dfe4bf2af2502651fd058f0 DE-627 ger DE-627 rakwb eng QB460-466 J. A. López-Vázquez verfasserin aut Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind. Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects Astrophysics Chin-Fei Lee verfasserin aut M. Fernández-López verfasserin aut Fabien Louvet verfasserin aut O. Guerra-Alvarado verfasserin aut Luis A. Zapata verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 28 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 28 https://doi.org/10.3847/1538-4357/ad132a kostenfrei https://doaj.org/article/acdf9ab14dfe4bf2af2502651fd058f0 kostenfrei https://doi.org/10.3847/1538-4357/ad132a 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 962 2024 1, p 28
spelling	10.3847/1538-4357/ad132a doi (DE-627)DOAJ09595998X (DE-599)DOAJacdf9ab14dfe4bf2af2502651fd058f0 DE-627 ger DE-627 rakwb eng QB460-466 J. A. López-Vázquez verfasserin aut Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind. Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects Astrophysics Chin-Fei Lee verfasserin aut M. Fernández-López verfasserin aut Fabien Louvet verfasserin aut O. Guerra-Alvarado verfasserin aut Luis A. Zapata verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 28 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 28 https://doi.org/10.3847/1538-4357/ad132a kostenfrei https://doaj.org/article/acdf9ab14dfe4bf2af2502651fd058f0 kostenfrei https://doi.org/10.3847/1538-4357/ad132a 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 962 2024 1, p 28
allfields_unstemmed	10.3847/1538-4357/ad132a doi (DE-627)DOAJ09595998X (DE-599)DOAJacdf9ab14dfe4bf2af2502651fd058f0 DE-627 ger DE-627 rakwb eng QB460-466 J. A. López-Vázquez verfasserin aut Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind. Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects Astrophysics Chin-Fei Lee verfasserin aut M. Fernández-López verfasserin aut Fabien Louvet verfasserin aut O. Guerra-Alvarado verfasserin aut Luis A. Zapata verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 28 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 28 https://doi.org/10.3847/1538-4357/ad132a kostenfrei https://doaj.org/article/acdf9ab14dfe4bf2af2502651fd058f0 kostenfrei https://doi.org/10.3847/1538-4357/ad132a 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 962 2024 1, p 28
allfieldsGer	10.3847/1538-4357/ad132a doi (DE-627)DOAJ09595998X (DE-599)DOAJacdf9ab14dfe4bf2af2502651fd058f0 DE-627 ger DE-627 rakwb eng QB460-466 J. A. López-Vázquez verfasserin aut Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind. Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects Astrophysics Chin-Fei Lee verfasserin aut M. Fernández-López verfasserin aut Fabien Louvet verfasserin aut O. Guerra-Alvarado verfasserin aut Luis A. Zapata verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 28 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 28 https://doi.org/10.3847/1538-4357/ad132a kostenfrei https://doaj.org/article/acdf9ab14dfe4bf2af2502651fd058f0 kostenfrei https://doi.org/10.3847/1538-4357/ad132a 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 962 2024 1, p 28
allfieldsSound	10.3847/1538-4357/ad132a doi (DE-627)DOAJ09595998X (DE-599)DOAJacdf9ab14dfe4bf2af2502651fd058f0 DE-627 ger DE-627 rakwb eng QB460-466 J. A. López-Vázquez verfasserin aut Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind. Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects Astrophysics Chin-Fei Lee verfasserin aut M. Fernández-López verfasserin aut Fabien Louvet verfasserin aut O. Guerra-Alvarado verfasserin aut Luis A. Zapata verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 28 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 28 https://doi.org/10.3847/1538-4357/ad132a kostenfrei https://doaj.org/article/acdf9ab14dfe4bf2af2502651fd058f0 kostenfrei https://doi.org/10.3847/1538-4357/ad132a 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 962 2024 1, p 28
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source	In The Astrophysical Journal 962(2024), 1, p 28 volume:962 year:2024 number:1, p 28
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author	J. A. López-Vázquez
spellingShingle	J. A. López-Vázquez misc QB460-466 misc Accretion misc Herbig-Haro objects misc Star formation misc Stellar winds misc Young stellar objects misc Astrophysics Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow
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topic_title	QB460-466 Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow Accretion Herbig-Haro objects Star formation Stellar winds Young stellar objects
topic	misc QB460-466 misc Accretion misc Herbig-Haro objects misc Star formation misc Stellar winds misc Young stellar objects misc Astrophysics
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title	Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow
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title_sort	multiple shells driven by disk winds: alma observations in the hh 30 outflow
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title_auth	Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow
abstract	We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind.
abstractGer	We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind.
abstract_unstemmed	We present archival Atacama Large Millimeter/submillimeter Array band 6 observations of the ^13 CO ( J = 2–1) and ^12 CO ( J = 2–1) molecular line emission of the protostellar system associated with HH 30. The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind.
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title_short	Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow
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The ^13 CO molecular line shows the accretion disk while the molecular outflow is traced by the emission of the ^12 CO molecular line. We estimated a dynamical mass for the central object of 0.45 ± 0.14 M _⊙ , and a mass for the molecular outflow of (1.83 ± 0.19) × 10 ^−4 M _⊙ . The molecular outflow presents an internal cavity as well as multiple outflowing shell structures. We distinguish three different shells with constant expansion (∼4–6 km s ^−1 ) and possible rotation signatures (≤0.5 km s ^−1 ). We find that the shells can be explained by magnetocentrifugal disk winds with launching radii R _launch ≲ 4 au and a small magnetic lever arm λ ∼ 1.6–1.9. The multiple shell structure may be the result of episodic ejections of the material from the accretion disk associated with three different epochs with dynamical ages of 497 ± 15 yr, 310 ± 9 yr, and 262 ± 11 yr for the first, second, and third shells, respectively. The outermost shell was ejected 187 ± 17 yr before the middle shell, while the middle shell was launched 48 ± 14 yr before the innermost shell. Our estimations of the linear and angular momentum rates of the outflow as well as the accretion luminosity are consistent with the values expected if the outflow of HH 30 is produced by a wide-angle disk wind.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Accretion</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Herbig-Haro objects</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Star formation</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar winds</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Young stellar objects</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Astrophysics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Chin-Fei Lee</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">M. 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Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow

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