The Ring Structure in the MWC 480 Disk Revealed by ALMA. (arXiv:1811.04074v1 [astro-ph.EP])

The Ring Structure in the MWC 480 Disk Revealed by ALMA. (arXiv:1811.04074v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Yao Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dipierro_G/0/1/0/all/0/1">Giovanni Dipierro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ragusa_E/0/1/0/all/0/1">Enrico Ragusa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lodato_G/0/1/0/all/0/1">Giuseppe Lodato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herczeg_G/0/1/0/all/0/1">Gregory J. Herczeg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Long_F/0/1/0/all/0/1">Feng Long</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harsono_D/0/1/0/all/0/1">Daniel Harsono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehler_Y/0/1/0/all/0/1">Yann Boehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menard_F/0/1/0/all/0/1">Francois Menard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_D/0/1/0/all/0/1">Doug Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pascucci_I/0/1/0/all/0/1">Ilaria Pascucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinilla_P/0/1/0/all/0/1">Paola Pinilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salyk_C/0/1/0/all/0/1">Colette Salyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plas_G/0/1/0/all/0/1">Gerrit van der Plas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrit_S/0/1/0/all/0/1">Sylvie Cabrit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_W/0/1/0/all/0/1">William J. Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hendler_N/0/1/0/all/0/1">Nathan Hendler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manara_C/0/1/0/all/0/1">Carlo F. Manara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nisini_B/0/1/0/all/0/1">Brunella Nisini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rigliaco_E/0/1/0/all/0/1">Elisabetta Rigliaco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avenhaus_H/0/1/0/all/0/1">Henning Avenhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banzatti_A/0/1/0/all/0/1">Andrea Banzatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gully_Santiago_M/0/1/0/all/0/1">Michael Gully-Santiago</a>

Gap-like structures in protoplanetary disks are likely related to planet
formation processes. In this paper, we present and analyze high resolution
(0.17*0.11 arcsec) 1.3 mm ALMA continuum observations of the protoplanetary
disk around the Herbig Ae star MWC 480. Our observations for the first time
show a gap centered at ~74au with a width of ~23au, surrounded by a bright ring
centered at ~98au from the central star. Detailed radiative transfer modeling
of both the ALMA image and the broadband spectral energy distribution is used
to constrain the surface density profile and structural parameters of the disk.
If the width of the gap corresponds to 4~8 times the Hill radius of a single
forming planet, then the putative planet would have a mass of 0.4~3 M_Jup. We
test this prediction by performing global three-dimensional smoothed particle
hydrodynamic gas/dust simulations of disks hosting a migrating and accreting
planet. We find that the dust emission across the disk is consistent with the
presence of an embedded planet with a mass of ~2.3 M_Jup at an orbital radius
of ~78au. Given the surface density of the best-fit radiative transfer model,
the amount of depleted mass in the gap is higher than the mass of the putative
planet, which satisfies the basic condition for the formation of such a planet.

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