Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities
Youdin, A. N.
Manara, C. F.
van der Plas, G.
Barenfeld, S. A.
Cox, E. G.
Hendler, N. P.
Pérez, L. M.
van der Marel, N.
AffiliationUniv Arizona, Dept Astron, Steward Observ
Univ Arizona, Lunar & Planetary Lab
Keywordsaccretion, accretion disks
planets and satellites: formation
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationP. Pinilla et al 2018 ApJ 859 32
Rights© 2018. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractWe analyze the dust morphology of 29 transition disks (TDs) observed with Atacama Large (sub-)Millimeter Array (ALMA) at (sub-)millimeter emission. We perform the analysis in the visibility plane to characterize the total flux, cavity size, and shape of the ring-like structure. First, we found that the M-dust-M-star relation is much flatter for TDs than the observed trends from samples of class II sources in different star-forming regions. This relation demonstrates that cavities open in high (dust) mass disks, independent of the stellar mass. The flatness of this relation contradicts the idea that TDs are a more evolved set of disks. Two potential reasons (not mutually exclusive) may explain this flat relation: the emission is optically thick or/and millimeter-sized particles are trapped in a pressure bump. Second, we discuss our results of the cavity size and ring width in the context of different physical processes for cavity formation. Photoevaporation is an unlikely leading mechanism for the origin of the cavity of any of the targets in the sample. Embedded giant planets or dead zones remain as potential explanations. Although both models predict correlations between the cavity size and the ring shape for different stellar and disk properties, we demonstrate that with the current resolution of the observations, it is difficult to obtain these correlations. Future observations with higher angular resolution observations of TDs with ALMA will help discern between different potential origins of cavities in TDs.
VersionFinal published version
SponsorsNASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51380.001-A]; NASA [NAS 5-26555]; DISCSIM project - European Research Council under ERC-ADG ; Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) [FOR 2634/1]; NSF Astronomy & Astrophysics Research Grant ; ESO Fellowship; ANR of France [ANR-16-CE31-0013]; National Science Foundation Graduate Research Fellowship [DGE1144469]; NSF [AST-1140063]