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Title: Rapid Evolution of Volatile CO from the Protostellar Disk Stage to the Protoplanetary Disk Stage
Award ID(s):
1907653
NSF-PAR ID:
10172402
Author(s) / Creator(s):
; ;
Date Published:
Journal Name:
The Astrophysical Journal
Volume:
891
Issue:
1
ISSN:
2041-8213
Page Range / eLocation ID:
L17
Format(s):
Medium: X
Sponsoring Org:
National Science Foundation
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  2. Abstract

    We study the kinematics of the AS 209 disk using theJ= 2–1 transitions of12CO,13CO, and C18O. We derive the radial, azimuthal, and vertical velocity of the gas, taking into account the lowered emission surface near the annular gap at ≃1.″7 (200 au) within which a candidate circumplanetary-disk-hosting planet has been reported previously. In12CO and13CO, we find a coherent upward flow arising from the gap. The upward gas flow is as fast as 150 m s−1in the regions traced by12CO 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 Elsässer number, Am, using the HCO+column density as a proxy for ion density and find that Am is ∼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.

     
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