On the diversity of asymmetries in gapped protoplanetary disks. (arXiv:2010.10568v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Marel_N/0/1/0/all/0/1">Nienke van der Marel</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Birnstiel_T/0/1/0/all/0/1">Til Birnstiel</a> (3,4), <a href="http://arxiv.org/find/astro-ph/1/au:+Garufi_A/0/1/0/all/0/1">Antonio Garufi</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Ragusa_E/0/1/0/all/0/1">Enrico Ragusa</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Christiaens_V/0/1/0/all/0/1">Valentin Christiaens</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Price_D/0/1/0/all/0/1">Daniel Price</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Sallum_S/0/1/0/all/0/1">Steph Sallum</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Muley_D/0/1/0/all/0/1">Dhruv Muley</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Francis_L/0/1/0/all/0/1">Logan Francis</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_R/0/1/0/all/0/1">Ruobing Dong</a> (1) ((1) University of Victoria, Canada, (2) Banting fellow, (3) LMU Muenchen, Germany, (4) Exzellenzcluster, Germany, (5) INAF, Italy, (6) University of Leicester, UK, (7) Monash University, Australia, (8) UC Irvine, USA)
Protoplanetary disks with large inner dust cavities are thought to host
massive planetary or substellar companions. These disks show asymmetries and
rings in the millimeter continuum, caused by dust trapping in pressure bumps,
and potentially vortices or horseshoes. The origin of the asymmetries and their
diversity remains unclear. We present a comprehensive study of 16 disks for
which the gas surface density profile has been constrained by CO isotopologue
data. We compare the azimuthal extents of the dust continuum profiles with the
local gas surface density in each disk, and find that the asymmetries
correspond to higher Stokes numbers or low gas surface density. We discuss
which asymmetric structures can be explained by a horseshoe, a vortex or spiral
density waves. Second, we reassess the gas gap radii from the $^{13}$CO maps,
which are about a factor 2 smaller than the dust ring radii, suggesting that
companions in these disks are in the brown dwarf mass regime ($sim 15-50
M_{rm Jup}$) or in the Super-Jovian mass regime ($sim 3-15 M_{rm Jup}$) on
eccentric orbits. This is consistent with the estimates from contrast curves on
companion mass limits. These curves rule out (sub)stellar companions ($q>$0.05)
for the majority of the sample at the gap location, but it remains possible at
even smaller radii. Third, we find that spiral arms in scattered light images
are primarily detected around high luminosity stars with disks with wide gaps,
which can be understood by the dependence of the spiral arm pitch angle on disk
temperature and companion mass.
Protoplanetary disks with large inner dust cavities are thought to host
massive planetary or substellar companions. These disks show asymmetries and
rings in the millimeter continuum, caused by dust trapping in pressure bumps,
and potentially vortices or horseshoes. The origin of the asymmetries and their
diversity remains unclear. We present a comprehensive study of 16 disks for
which the gas surface density profile has been constrained by CO isotopologue
data. We compare the azimuthal extents of the dust continuum profiles with the
local gas surface density in each disk, and find that the asymmetries
correspond to higher Stokes numbers or low gas surface density. We discuss
which asymmetric structures can be explained by a horseshoe, a vortex or spiral
density waves. Second, we reassess the gas gap radii from the $^{13}$CO maps,
which are about a factor 2 smaller than the dust ring radii, suggesting that
companions in these disks are in the brown dwarf mass regime ($sim 15-50
M_{rm Jup}$) or in the Super-Jovian mass regime ($sim 3-15 M_{rm Jup}$) on
eccentric orbits. This is consistent with the estimates from contrast curves on
companion mass limits. These curves rule out (sub)stellar companions ($q>$0.05)
for the majority of the sample at the gap location, but it remains possible at
even smaller radii. Third, we find that spiral arms in scattered light images
are primarily detected around high luminosity stars with disks with wide gaps,
which can be understood by the dependence of the spiral arm pitch angle on disk
temperature and companion mass.
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