Abstract
Abstract Protoplanets can produce structures in protoplanetary disks via gravitational disk–planet interactions. Once detected, such structures serve as signposts of planet formation. Here we investigate the kinematic signatures in disks produced by multi-Jupiter mass (M J) planets using 3D hydrodynamics and radiative transfer simulations. Such a planet opens a deep gap, and drives transonic vertical motions inside. Such motions include both a bulk motion of the entire half-disk column, and turbulence on scales comparable to and smaller than the scale height. They significantly broaden molecular lines from the gap, producing double-peaked line profiles at certain locations, and a kinematic velocity dispersion comparable to thermal after azimuthal averaging. The same planet does not drive fast vertical motions outside the gap, except at the inner spiral arms and the disk surface. Searching for line broadening induced by multi-M J planets inside gaps requires an angular resolution comparable to the gap width, an assessment of the gap gas temperature to within a factor of 2, and a high sensitivity needed to detect line emission from the gap.
Highlights
Detecting protoplanets forming in protoplanetary disks provides fundamental constraints on key parameters governing the planet formation processes, such as location, timescale, and local environment
Perez et al (2018) investigated gas kinematics caused by pressure gradients at gaps, spiral wakes and vortices. While these works mainly focused on planet-induced signatures in intensity weighted velocity maps1, we study how meridional motions are manifested in velocity dispersion maps
In this paper we use 3D hydrodynamics and radiative transfer simulations to study the signatures of planetinduced turbulence in gaps in gas line observations
Summary
Detecting protoplanets forming in protoplanetary disks provides fundamental constraints on key parameters governing the planet formation processes, such as location, timescale, and local environment. The two flows connect via meridional circulations, which can reach velocities comparable to local sound speed cs in gaps opened by super-Jupiter planets (Fung & Chiang 2016) These gas motions may significantly broaden molecular emission lines. In a pioneering work, Perez et al (2015) assessed the detectability of the rotation of CPDs. More recently, Pinte et al (2018) showed that a planet may introduce local kinks in the isovelocity maps of the circumstellar disk, Teague et al (2018a) quantified the radial modulation in the circumstellar disk rotation due to gap structures, and Huang et al (2018b) studied the detectability of the anticyclonic gas motion inside planettriggered vortices. A generic strategy in searching for such signatures in real observations is outlined (§5), and advantages of those signatures as signposts of planets are highlighted (§5.1)
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