Observational Signatures of Planets in Protoplanetary Disks: Planet-Induced Line Broadening in Gaps. (arXiv:1811.09629v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dong_R/0/1/0/all/0/1">Ruobing Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">Sheng-yuan Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fung_J/0/1/0/all/0/1">Jeffrey Fung</a>
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 ($M_{rm J}$) 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-$M_{rm J}$ 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.
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 ($M_{rm J}$) 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-$M_{rm J}$ 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.
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