Molecules with ALMA at Planet-forming Scales (MAPS). XVI. Characterizing the Impact of the Molecular Wind on the Evolution of the HD 163296 System

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dc.contributor.authorBooth, Alice S.
dc.contributor.authorTabone, Benoit
dc.contributor.authorIlee, John D.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorAikawa, Yuri
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorBae, Jaehan
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorBergner, Jennifer B.
dc.contributor.authorBosman, Arthur D.
dc.contributor.authorCalahan, Jenny K.
dc.contributor.authorCataldi, Gianni
dc.contributor.authorCleeves, L. Ilsedore
dc.contributor.authorCzekala, Ian
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorHuang, Jane
dc.contributor.authorLaw, Charles J.
dc.contributor.authorLe Gal, Romane
dc.contributor.authorLong, Feng
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorMenard, Francois
dc.contributor.authorNomura, Hideko
dc.contributor.authorOberg, Karin, I
dc.contributor.authorQi, Chunhua
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorTeague, Richard
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorWilner, David J.
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorZhang, Ke
dc.date.accessioned2025-01-20T22:05:49Z
dc.date.available2025-01-20T22:05:49Z
dc.date.issued2021
dc.description.abstractDuring the main phase of evolution of a protoplanetary disk, accretion regulates the inner-disk properties, such as the temperature and mass distribution, and in turn, the physical conditions associated with planet formation. The driving mechanism behind accretion remains uncertain; however, one promising mechanism is the removal of a fraction of angular momentum via a magnetohydrodynamic (MHD) disk wind launched from the inner tens of astronomical units of the disk. This paper utilizes CO isotopologue emission to study the unique molecular outflow originating from the HD 163296 protoplanetary disk obtained with the Atacama Large Millimeter/submillimeter Array. HD 163296 is one of the most well-studied Class II disks and is proposed to host multiple gas-giant planets. We robustly detect the large-scale rotating outflow in the (CO)-C-12 J = 2 - 1 and the (CO)-C-13 J = 2 - 1 and J = 1 - 0 transitions. We constrain the kinematics, the excitation temperature of the molecular gas, and the mass-loss rate. The high ratio of the rates of ejection to accretion (5-50), together with the rotation signatures of the flow, provides solid evidence for an MHD disk wind. We find that the angular momentum removal by the wind is sufficient to drive accretion though the inner region of the disk; therefore, accretion driven by turbulent viscosity is not required to explain HD 163296's accretion. The low temperature of the molecular wind and its overall kinematics suggest that the MHD disk wind could be perturbed and shocked by the previously observed high-velocity atomic jet. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac1ad4
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac1ad4
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94169
dc.identifier.wosidWOS:000714224400001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). XVI. Characterizing the Impact of the Molecular Wind on the Evolution of the HD 163296 System
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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