Ring structure in the MWC 480 disk revealed by ALMA

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′′) 1.3 mm ALMA continuum observations of the protoplanetary disk around the Herbig Ae star MWC 480. Our observations show for the first ti...

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Published in:Astronomy and astrophysics (Berlin) 2019-02, Vol.622, p.A75
Main Authors: Liu, Yao, Dipierro, Giovanni, Ragusa, Enrico, Lodato, Giuseppe, Herczeg, Gregory J., Long, Feng, Harsono, Daniel, Boehler, Yann, Menard, Francois, Johnstone, Doug, Pascucci, Ilaria, Pinilla, Paola, Salyk, Colette, van der Plas, Gerrit, Cabrit, Sylvie, Fischer, William J., Hendler, Nathan, Manara, Carlo F., Nisini, Brunella, Rigliaco, Elisabetta, Avenhaus, Henning, Banzatti, Andrea, Gully-Santiago, Michael
Format: Article
Language:English
Subjects:
Accretion disks
Astrophysics
Broadband
Computer simulation
Density
Deposition
Dust
Physics
Planet formation
planet-disk interactions
protoplanetary disks
Protoplanets
Radiative transfer
Ring structures
Spectral energy distribution
stars: formation
stars: individual: MWC 480
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Summary: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′′) 1.3 mm ALMA continuum observations of the protoplanetary disk around the Herbig Ae star MWC 480. Our observations show for the first time a gap centered at ~74 au with a width of ~23 au, surrounded by a bright ring centered at ~98 au from the central star. Detailed radiative transfer modeling of 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 MJ. 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 MJ at an orbital radius of ~78 au. 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.
ISSN:0004-6361
1432-0746
1432-0756
DOI:10.1051/0004-6361/201834157