The Ophiuchus DIsc Survey Employing ALMA (ODISEA) – III. The evolution of substructures in massive discs at 3–5 au resolution

2020/12/05 by Lucas A. Cieza, Camilo González-Ruilova, Antonio S. Hales +21 · 128 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Molecular Spectroscopy and Structure #Molecular cloud #Ophiuchus #Physics #Planet #Population #Protostar #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph.EP #astro-ph.SR

paper · pdf · doi:10.1093/mnras/staa3787

published in Monthly Notices of the Royal Astronomical Society 501(2), 2934-2953 (Oxford University Press) · 21 pages, 10 figures. Appendix with 3 additional figures. Version 2, identical to previous one, but now accepted for publication (in MNRAS)

arxiv created 2020/12/05 · openalex created_date 2020/12/07 · openalex publication_date 2020/12/08 · arxiv updated 2020/12/16 · openalex updated_date 2026/08/05

Abstract

ABSTRACT We present 1.3 mm continuum ALMA long-baseline observations at 3–5 au resolution of 10 of the brightest discs from the Ophiuchus DIsc Survey Employing ALMA (ODISEA) project. We identify a total of 26 narrow rings and gaps distributed in 8 sources and 3 discs with small dust cavities (r <10 au). We find that two discs around embedded protostars lack the clear gaps and rings that are ubiquitous in more evolved sources with Class II SEDs. Our sample includes five objects with previously known large dust cavities (r >20 au). We find that the 1.3 mm radial profiles of these objects are in good agreement with those produced by numerical simulations of dust evolution and planet–disc interactions, which predict the accumulation of mm-sized grains at the edges of planet-induced cavities. Our long-baseline observations resulted in the largest sample of discs observed at ∼3–5 au resolution in any given star-forming region (15 objects when combined with Ophiuchus objects in the DSHARP Large Program) and allow for a demographic study of the brightest ∼ 5 \rm per cent of the discs in Ophiuchus (i.e. the most likely formation sites of giant planets in the cloud). We use this unique sample to propose an evolutionary sequence and discuss a scenario in which the substructures observed in massive protoplanetary discs are mainly the result of planet formation and dust evolution. If this scenario is correct, the detailed study of disc substructures might provide a window to investigate a population of planets that remains mostly undetectable by other techniques.

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Cited by

• A population of transition disks around evolved stars: Fingerprints of planets
• Linking Outer Disk Pebble Dynamics and Gaps to Inner Disk Water Enrichment