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Cited by 709Astrophysics and Star Formation StudiesAstro and Planetary ScienceStellar, planetary, and galactic studies

The DOI matches its Crossref record; 165 of the 168 references it cites were found in a registry or an index.

PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS

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Andrews, Sean M., Wilner, D. J., Hughes, A. M., Qi, Chunhua, Dullemond, C. P.·2009·The Astrophysical Journal
DOI 10.1088/0004-637x/700/2/1502
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Abstract

We present the results of a high angular resolution (0 3 ≈ 40 AU) Submillimeter Array survey of the 345 GHz (870 μm) thermal continuum emission from nine of the brightest, and therefore most massive, circumstellar disks in the ∼1 Myr-old Ophiuchus star-forming region. Using two-dimensional radiative transfer calculations, we simultaneously fit the observed continuum visibilities and broadband spectral energy distribution for each disk with a parametric structure model. Compared to previous millimeter studies, this survey includes significant upgrades in modeling, data quality, and angular resolution that provide improved constraints on key structure parameters, particularly those that characterize the spatial distribution of mass in the disks. In the context of a surface density profile motivated by similarity solutions for viscous accretion disks, Σ ∝ ( R / R c ) −γ exp [ − ( R / R c ) 2−γ ], the best-fit models for the sample disks have characteristic radii R c ≈ 20–200 AU, high disk masses M d ≈ 0.005–0.14 M ☉ (a sample selection bias), and a narrow range of radial Σ gradients (γ ≈ 0.4–1.0) around a median γ = 0.9. These density structures are used in conjunction with accretion rate estimates from the literature to help characterize the viscous evolution of the disk material. Using the standard prescription for disk viscosities, those combined constraints indicate that α ≈ 0.0005–0.08. Three of the sample disks show large ( R ≈ 20–40 AU) central cavities in their continuum emission morphologies, marking extensive zones where dust has been physically removed and/or has significantly diminished opacities. Based on the current requirements of planet formation models, these emission cavities and the structure constraints for the sample as a whole suggest that these young disks may eventually produce planetary systems, and have perhaps already started.

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Citations

Cites

Research works printed but not linked: 22

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  5. Cutri, 2003, 2MASS All-Sky Point Source Catalog
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Metadata

Authors
Andrews, S. M., Wilner, D. J., Hughes, A. M., Qi, C., & Dullemond, C. P.
Affiliations
  • Center for Astrophysics Harvard & Smithsonian (US)
  • Max Planck Institute for Astronomy (DE)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2009-07-14
Volume
700
Issue
2
Pages
1502-1523
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/700/2/1502
OpenAlex
W2047712469
Cited by
709
References
168
Citations by year
2026: 16 · 2025: 22 · 2024: 21 · 2023: 21 · 2022: 25 · 2021: 30 · 2020: 43 · 2019: 45 · 2018: 90 · 2017: 59 · 2016: 71 · 2015: 48 · 2014: 37 · 2013: 56 · 2012: 40
FWCI
21.00
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Max Planck Institute for Plasma Physics (submittedVersion)
  • arXiv (Cornell University)
Funders
  • National Aeronautics and Space Administration (NNG05GI81G, NAS 526555, 526555)
  • Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords
protoplanetary disks, Ophiuchus star-forming region, disk structure, surface density profile, disk mass, disk viscosity, accretion rate, disk cavity, dust removal, planet formation, radiative transfer modeling

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