Ring structure in the MWC 480 disk revealed by ALMA

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

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Ring structure in the MWC 480 disk revealed by ALMA

MPS-Authors

Liu, Yao
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dipierro, Giovanni
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ragusa, Enrico
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lodato, Giuseppe
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Herczeg, Gregory J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Long, Feng
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Harsono, Daniel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Boehler, Yann
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Menard, Francois
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Johnstone, Doug
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pascucci, Ilaria
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pinilla, Paola
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Salyk, Colette
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van der Plas, Gerrit
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cabrit, Sylvie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fischer, William J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hendler, Nathan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Manara, Carlo F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Nisini, Brunella
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rigliaco, Elisabetta
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Avenhaus, Henning
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Banzatti, Andrea
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gully-Santiago, Michael
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2019A&A...622A..75L
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Citation

Liu, Y., Dipierro, G., Ragusa, E., Lodato, G., Herczeg, G. J., Long, F., et al. (2019). Ring structure in the MWC 480 disk revealed by ALMA. Astronomy and Astrophysics, 622.

Cite as: https://hdl.handle.net/21.11116/0000-0005-D325-3

Abstract

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 M_J. 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_J 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. The reduced image (FITS file) is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/622/A75">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/622/A75</A>.