Molecules with ALMA at Planet-forming Scales (MAPS): Complex Kinematics in the AS 209 Disk Induced by a Forming Planet and Disk Winds

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dc.contributor.authorGalloway-Sprietsma, Maria
dc.contributor.authorBae, Jaehan
dc.contributor.authorTeague, Richard
dc.contributor.authorBenisty, Myriam
dc.contributor.authorFacchini, Stefano
dc.contributor.authorAikawa, Yuri
dc.contributor.authorAlarcon, Felipe
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorBergin, Edwin
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.authorLiu, Yao
dc.contributor.authorLong, Feng
dc.contributor.authorMenard, Francois
dc.contributor.authorOberg, Karin I.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorWilner, David J.
dc.date.accessioned2025-01-20T20:08:56Z
dc.date.available2025-01-20T20:08:56Z
dc.date.issued2023
dc.description.abstractWe study the kinematics of the AS 209 disk using the J = 2-1 transitions of (CO)-C-12, (CO)-C-13, and (CO)-O-18. We derive the radial, azimuthal, and vertical velocity of the gas, taking into account the lowered emission surface near the annular gap at similar or equal to 1.'' 7 (200 au) within which a candidate circumplanetary-disk-hosting planet has been reported previously. In (CO)-C-12 and (CO)-C-13, we find a coherent upward flow arising from the gap. The upward gas flow is as fast as 150 m s(-1) in the regions traced by (CO)-C-12 emission, which corresponds to about 50% of the local sound speed or 6% of the local Keplerian speed. Such an upward gas flow is difficult to reconcile with an embedded planet alone. Instead, we propose that magnetically driven winds via ambipolar diffusion are triggered by the low gas density within the planet-carved gap, dominating the kinematics of the gap region. We estimate the ambipolar Elsasser number, Am, using the HCO+ column density as a proxy for ion density and find that Am is similar to 0.1 at the radial location of the upward flow. This value is broadly consistent with the value at which numerical simulations find that ambipolar diffusion drives strong winds. We hypothesize that the activation of magnetically driven winds in a planet-carved gap can control the growth of the embedded planet. We provide a scaling relationship that describes the wind-regulated terminal mass: adopting parameters relevant to 100 au from a solar-mass star, we find that the wind-regulated terminal mass is about one Jupiter mass, which may help explain the dearth of directly imaged super-Jovian-mass planets.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/accae4
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/accae4
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/91951
dc.identifier.wosidWOS:001010411600001
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS): Complex Kinematics in the AS 209 Disk Induced by a Forming Planet and Disk Winds
dc.typeartículo
dc.volumen950
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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