TY - JOUR
T1 - Ring structure in the MWC 480 disk revealed by ALMA
AU - Liu, Yao
AU - Dipierro, Giovanni
AU - Ragusa, Enrico
AU - Lodato, Giuseppe
AU - Herczeg, Gregory J.
AU - Long, Feng
AU - Harsono, Daniel
AU - Boehler, Yann
AU - Menard, Francois
AU - Johnstone, Doug
AU - Pascucci, Ilaria
AU - Pinilla, Paola
AU - Salyk, Colette
AU - Van Der Plas, Gerrit
AU - Cabrit, Sylvie
AU - Fischer, William J.
AU - Hendler, Nathan
AU - Manara, Carlo F.
AU - Nisini, Brunella
AU - Rigliaco, Elisabetta
AU - Avenhaus, Henning
AU - Banzatti, Andrea
AU - Gully-Santiago, Michael
N1 - Funding Information:
D.H. is supported by European Union A-ERC grant 291141 CHEMPLAN, NWO and by a KNAW professor prize awarded to E. van Dishoeck. Y.B., F.M. and G.v.d.P. acknowledge funding from ANR of France under contract number ANR-16-CE31-0013. D.J. is supported by NRC Canada and by an NSERC Discovery Grant. C.F.M. acknowledges an ESO Fellowship. This research used the ALICE High Performance Computing Facility and the DiRAC Data Intensive service operated by the University of Leicester IT Services. These resources form part of the STFC DiRAC HPC Facility (www.dirac.ac.uk), jointly funded by STFC and the Large Facilities Capital Fund of BIS via STFC capital grants ST/K000373/1 and ST/R002363/1 and STFC DiRAC Operations grant ST/R001014/1. This paper makes use of the following ALMA data: 2016.1.01164.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Funding Information:
Acknowledgements. Y.L. acknowledges supports by the Natural Science Foundation of Jiangsu Province of China (Grant No. BK20181513) and by the Natural Science Foundation of China (Grant No. 11503087). G.D. acknowledges financial support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 681601). G.L. and B.N. thank the support by the project PRIN-INAF 2016 The Cradle of Life – GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA). G.J.H. is supported by general grants 11473005 and 11773002 awarded by the National Science Foundation of China.
Publisher Copyright:
© ESO 2019.
PY - 2019/2/1
Y1 - 2019/2/1
N2 - 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.
AB - 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.
KW - Protoplanetary disks
KW - planet-disk interactions
KW - radiative transfer
KW - stars: formation
KW - stars: individual: MWC 480
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UR - http://www.scopus.com/inward/citedby.url?scp=85060972374&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201834157
DO - 10.1051/0004-6361/201834157
M3 - Article
AN - SCOPUS:85060972374
SN - 0004-6361
VL - 622
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A75
ER -