Models of the dust structures around Vega-excess stars
Open accessAbstract
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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Self-citationFirst Detection of Millimeter Dust Emission from Brown Dwarf Disks
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Kuiper belts around nearby stars
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MODELING THE HD 32297 DEBRIS DISK WITH FAR-INFRARED HERSCHEL DATA
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A 25 micron search for Vega-like disks around main-sequence stars with ISO
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APOCENTER GLOW IN ECCENTRIC DEBRIS DISKS: IMPLICATIONS FOR FOMALHAUT AND ϵ ERIDANI
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MILLIMETER IMAGING OF THE β PICTORIS DEBRIS DISK: EVIDENCE FOR A PLANETESIMAL BELT
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Search for cold debris disks around M-dwarfs. II
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PLANETESIMALS IN DEBRIS DISKS OF SUN-LIKE STARS
Shannon, A., & Wu, Y. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/739/1/36 · Cited by 55 · see citing works
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Long-Lived Planetesimal DiscsPreprint
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Detecting protoplanets with ALMA
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The 1.2 mm image of theβPictoris disk
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“For debris disks, a collisional cascade from a reservoir of large bodies generates micron sized material that is seen in reflected light observations (Backman & Paresce 1993; Dent et al. 2000).”
BackgroundVLT imaging of theβ Pictoris gas disk
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- Authors
- Dent, W. R. F., Walker, H. J., Holland, W. S., & Greaves, J. S.
- Affiliations
- Royal Observatory (GB)
- 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
- 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
- bronze
- doi.org
- 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 › Physics and Astronomy › Astronomy and Astrophysics › 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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