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Cited by 128Astrophysics and Star Formation StudiesStellar, planetary, and galactic studiesAstro and Planetary Science

The DOI matches its Crossref record; 37 of the 37 references it cites were found in a registry or an index.

Models of the dust structures around Vega-excess stars

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Dent, W. R. F., Walker, H. J., Holland, W. S., Greaves, J. S.·2000·Monthly Notices of the Royal Astronomical Society
DOI 10.1046/j.1365-8711.2000.03331.x
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Abstract

We present models of the submillimetre dust emission around four Vega-excess stars. The results are adjusted to fit simultaneously the spectral energy distribution from millimetre through to optical wavelengths, as well as the submillimetre image. The combination of spatially resolved images with continuum fluxes over a range of wavelengths can remove some of the previous ambiguities in estimating the dust emission characteristics and circumstellar distributions. Fomalhaut shows the brightest and best-resolved submillimetre image, and so gives the most unambiguous fit. Both the imaging and photometric results can best be modelled by an edge-on thick torus, of inner radius 100 au, outer radius 140 au and thickness ∼120 au. The observed sharp outer boundary cannot be fitted by a reasonable power-law density distribution. Furthermore, inside 100 au the density also drops abruptly, by at least a factor of 10. The structures of Vega and ε Eri are also best modelled by radially thin rings rather than discs, in both cases viewed almost pole-on. However, there are clearly clumps in their morphologies which cannot be explained by simple axisymmetric models. The submillimetre disc in β Pic can be adequately fitted by the same model as that used to account for the extended structure seen in scattered light. However, the additional south-western emission component, if it lies in the β Pic system, must have a dust mass comparable to that of the whole visible disc. In all cases, the spectral energy distribution can be fitted by a single ring or disc-like structure. Grain sizes of a few tens of μm and β=0.8–1.1 provide the best fits, and we place limits on the dust size distribution. The dust temperatures are too low and there is too much temperature variation between the sources for grain sublimation to be effective at creating the central holes. All rings are dominated by grain-grain collisions, and we discuss methods of creating and sustaining the observed structures. Most likely they arise from a mechanism such as planet shepherding. The outer cut-off may arise in a similar way, although external stripping of material is not discounted.

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  1. 1999, AA, 348, 557
  2. 1998, AA, 339, 831
  3. 1990, AA, 227, 5L
  4. 1991, AA, 252, 220
  5. 1998, AA, 329, 53L
  6. 1998, AA, 331, 291
  7. 1996, ASP CONF SER, 104, 163
  8. 1998, AA, 337, 808
  9. 1997, AA, 327, 1123
  10. 1994, AA, 285, 229

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Metadata

Authors
Dent, W. R. F., Walker, H. J., Holland, W. S., & Greaves, J. S.
Affiliations
Royal Observatory (GB)
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2000-06-01
Volume
314
Issue
4
Pages
702-712
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1046/j.1365-8711.2000.03331.x
OpenAlex
W2111511689
Cited by
128
References
37
Citations by year
2025: 1 · 2019: 2 · 2018: 1 · 2017: 4 · 2016: 5 · 2015: 1 · 2014: 3 · 2013: 4 · 2012: 7
FWCI
5.68
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • Science and Technology Facilities Council (submittedVersion)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
Keywords
circumstellar dust, Fomalhaut, Vega, epsilon Eridani, Beta Pictoris, spectral energy distribution, grain size distribution, dust temperature, scattered light

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