Mapping the 3D Kinematical Structure of the Gas Disk of HD 169142

Abstract

The disk around HD 169142 has been suggested to host multiple embedded planets due to the range of structures observed in the dust distributions. We analyze archival ALMA observations of ${}^{12}\mathrm{CO}(2-1)$, ${}^{13}\mathrm{CO}(2-1)$, and ${\mathrm{C}}^{18}\mathrm{O}(2-1)$ to search for large-scale kinematic structures associated with other embedded planets in the outer disk. At 125 au, we identify a coherent flow from the disk surface to the midplane, traced by all three CO isotopologues, and interpret it as a meridional flow, potentially driven by an embedded planet. We use changes in the rotation speed of the gas to characterize the physical structure across this region, finding that at 125 au the CO emission traces regions of increased gas pressure, despite being at a surface density minimum. Developing a simple analytical model, we demonstrate that the physical structure of the gap can have non-trivial responses to changes in the surface density, consistent both with previous thermo-chemical models, and the conditions inferred observationally. Applying this technique to a range of sources will allow us to directly confront theoretical models of gap-opening in protoplanetary disks.

23 pages, 17 figures, accepted for publication in ApJL

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Cited by in corpus (6)

• Kinematics and brightness temperatures of transition discs -- A survey of gas substructures as seen with ALMA
• Accreting protoplanets: Spectral signatures and magnitude of gas and dust extinction at H alpha
• Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission
• A localized kinematic structure detected in atomic carbon emission spatially coincident with a proposed protoplanet in the HD 163296 disk
• Probing inner and outer disk misalignments in transition disks
• CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks