Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multiwavelength Atacama Large Millimeter/submillimeter Array Observations

DOI: 
10.3847/1538-4357/ab31a2
Publication date: 
01/08/2019
Main author: 
Macías, Enrique
IAA authors: 
Osorio, Mayra;Anglada, Guillem;Gómez, José F.
Authors: 
Macías, Enrique;Espaillat, Catherine C.;Osorio, Mayra;Anglada, Guillem;Torrelles, José M.;Carrasco-González, Carlos;Flock, Mario;Linz, Hendrik;Bertrang, Gesa H. -M.;Henning, Thomas;Gómez, José F.;Calvet, Nuria;Dent, William R. F.
Journal: 
The Astrophysical Journal
Refereed: 
Yes
Publication type: 
Article
Volume: 
881
Pages: 
159
Abstract: 
We present a detailed multiwavelength characterization of the multi-ring disk of HD 169142. We report new Atacama Large Millimeter/submillimeter Array (ALMA) observations at 3 mm and analyze them together with archival 0.89 and 1.3 mm data. Our observations resolve three out of the four rings in the disk previously seen in high-resolution ALMA data. A simple parametric model is used to estimate the radial profile of the dust optical depth, temperature, density, and particle size distribution. We find that the multiple ring features of the disk are produced by annular accumulations of large particles, probably associated with gas pressure bumps. Our model indicates that the maximum dust grain size in the rings is ∼1 cm, with slightly flatter power-law size distributions than the interstellar medium-like size distribution (p ∼ 3.5) found in the gaps. In particular, the inner ring (∼26 au) is associated with a strong and narrow buildup of dust particles that could harbor the necessary conditions to trigger the streaming instability. According to our analysis, the snowlines of the most important volatiles do not coincide with the observed substructures. We explore different ring formation mechanisms and find that planet─disk interactions are the most likely scenario to explain the main features of HD 169142. Overall, our multiwavelength analysis provides some of the first unambiguous evidence of the presence of radial dust traps in the rings of HD 169142. A similar analysis in a larger sample of disks could provide key insights on the impact that disk substructures have on the dust evolution and planet formation processes.
Database: 
ADS
SCOPUS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85072310349&doi=10.3847%2f1538-4357%2fab31a2&partnerID=40&md5=6e6601c75c4abd913ad31a3053411661
ADS Bibcode: 
2019ApJ...881..159M
Keywords: 
planet─disk interactions;protoplanetary disks;stars: individual: HD 169142;stars: pre-main sequence;techniques: interferometric;Astrophysics - Solar and Stellar Astrophysics;Astrophysics - Earth and Planetary Astrophysics;Astrophysics - Astrophysics of Galaxies