The Disk Substructures at High Angular Resolution Project (DSHARP): VII. The Planet-Disk Interactions Interpretation. (arXiv:1812.04045v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shangjia Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Z/0/1/0/all/0/1">Zhaohuan Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">Jane Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzman_V/0/1/0/all/0/1">Viviana V. Guzmán</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_S/0/1/0/all/0/1">Sean M. Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birnstiel_T/0/1/0/all/0/1">Tilman Birnstiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dullemond_C/0/1/0/all/0/1">Cornelis P. Dullemond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">Andrea Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_L/0/1/0/all/0/1">Laura M. Pérez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benisty_M/0/1/0/all/0/1">Myriam Benisty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David J. Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baruteau_C/0/1/0/all/0/1">Clément Baruteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xue-Ning Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>
The Disk Substructures at High Angular Resolution Project (DSHARP) provides a
large sample of protoplanetary disks having substructures which could be
induced by young forming planets. To explore the properties of planets that may
be responsible for these substructures, we systematically carry out a grid of
2-D hydrodynamical simulations including both gas and dust components. We
present the resulting gas structures, including the relationship between the
planet mass and 1) the gaseous gap depth/width, and 2) the sub/super-Keplerian
motion across the gap. We then compute dust continuum intensity maps at the
frequency of the DSHARP observations. We provide the relationship between the
planet mass and 1) the depth/width of the gaps at millimeter intensity maps, 2)
the gap edge ellipticity and asymmetry, and 3) the position of secondary gaps
induced by the planet. With these relationships, we lay out the procedure to
constrain the planet mass using gap properties, and study the potential planets
in the DSHARP disks. We highlight the excellent agreement between observations
and simulations for AS 209 and the detectability of the young Solar System
analog. Finally, under the assumption that the detected gaps are induced by
young planets, we characterize the young planet population in the planet
mass-semimajor axis diagram. We find that the occurrence rate for $>$ 5 $M_J$
planets beyond 5-10 au is consistent with direct imaging constraints. Disk
substructures allow us probe a wide-orbit planet population (Neptune to Jupiter
mass planets beyond 10 au) that is not accessible to other planet searching
techniques.
The Disk Substructures at High Angular Resolution Project (DSHARP) provides a
large sample of protoplanetary disks having substructures which could be
induced by young forming planets. To explore the properties of planets that may
be responsible for these substructures, we systematically carry out a grid of
2-D hydrodynamical simulations including both gas and dust components. We
present the resulting gas structures, including the relationship between the
planet mass and 1) the gaseous gap depth/width, and 2) the sub/super-Keplerian
motion across the gap. We then compute dust continuum intensity maps at the
frequency of the DSHARP observations. We provide the relationship between the
planet mass and 1) the depth/width of the gaps at millimeter intensity maps, 2)
the gap edge ellipticity and asymmetry, and 3) the position of secondary gaps
induced by the planet. With these relationships, we lay out the procedure to
constrain the planet mass using gap properties, and study the potential planets
in the DSHARP disks. We highlight the excellent agreement between observations
and simulations for AS 209 and the detectability of the young Solar System
analog. Finally, under the assumption that the detected gaps are induced by
young planets, we characterize the young planet population in the planet
mass-semimajor axis diagram. We find that the occurrence rate for $>$ 5 $M_J$
planets beyond 5-10 au is consistent with direct imaging constraints. Disk
substructures allow us probe a wide-orbit planet population (Neptune to Jupiter
mass planets beyond 10 au) that is not accessible to other planet searching
techniques.
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