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
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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Citations
Cites
The size distribution of interstellar grains
Mathis, J. S., Rumpl, W. M., & Nordsieck, K. H. (1977) · The Astrophysical Journal · doi:10.1086/155591 · Cited by 3,879
(1993) · Choice Reviews Online · doi:10.5860/choice.31-2093 · Cited by 2,161
Lin, D. N. C., & Papaloizou, J. (1986) · The Astrophysical Journal · doi:10.1086/164653 · Cited by 1,054
A Circumstellar Disk Around β Pictoris
Smith, B. A., & Terrile, R. J. (1984) · Science · doi:10.1126/science.226.4681.1421 · Cited by 735
Discovery of a shell around Alpha Lyrae
Aumann, H. H., Beichman, C. A., Gillett, F. C., de Jong, T., Houck, J. R., Low, F. J., Neugebauer, G. X., Walker, R. G., & Wesselius, P. R. (1984) · The Astrophysical Journal · doi:10.1086/184214 · Cited by 625
Submillimetre images of dusty debris around nearby stars
Holland, W. S., Greaves, J. S., Zuckerman, B., Webb, R. A., McCarthy, C., Coulson, I. M., Walther, D. M., Dent, W. R. F., Gear, W. K., & Robson, I. E. (1998) · Nature · doi:10.1038/33874 · Cited by 431
Self-citationA Dust Ring around ε Eridani: Analog to the Young Solar System
Greaves, J. S., Holland, W. S., Moriarty-Schieven, G. H., Jenness, T., Dent, W. R. F., Zuckerman, B., McCarthy, C., Webb, R. A., Butner, H. M., Gear, W. K., et al. (1998) · The Astrophysical Journal · doi:10.1086/311652 · Cited by 337
Self-citationNICMOS Imaging of the HR 4796A Circumstellar Disk
Schneider, G., Smith, B. A., Becklin, E. E., Koerner, D. W., Meier, R., Hines, D. C., Lowrance, P., Terrile, R. J., Thompson, R. I., & Rieke, M. J. (1999) · The Astrophysical Journal · doi:10.1086/311921 · Cited by 270
Störzer, H., & Hollenbach, D. J. (1999) · The Astrophysical Journal · doi:10.1086/307055 · Cited by 233
A circumstellar dust disk around a star with a known planetary companion
Trilling, D. E., & Brown, R. H. (1998) · Nature · doi:10.1038/27389 · Cited by 231
Research works printed but not linked: 10
- 1999, AA, 348, 557
- 1998, AA, 339, 831
- 1990, AA, 227, 5L
- 1991, AA, 252, 220
- 1998, AA, 329, 53L
- 1998, AA, 331, 291
- 1996, ASP CONF SER, 104, 163
- 1998, AA, 337, 808
- 1997, AA, 327, 1123
- 1994, AA, 285, 229
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Imaging Extrasolar Giant Planets
Bowler, B. P. (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/968/102001 · Cited by 450
A planetary system as the origin of structure in Fomalhaut's dust belt
Kalas, P., Graham, J. R., & Clampin, M. (2005) · Nature · doi:10.1038/nature03601 · Cited by 411
Debris Disk Evolution around A Stars
Su, K. Y. L., Rieke, G. H., Stansberry, J. A., Bryden, G., Stapelfeldt, K. R., Trilling, D. E., Muzerolle, J., Beichman, C. A., Moro‐Martin, A., Hines, D. C., et al. (2006) · The Astrophysical Journal · doi:10.1086/508649 · Cited by 385
Frequency of Debris Disks around Solar‐Type Stars: First Results from aSpitzerMIPS Survey
Bryden, G., Beichman, C., Trilling, D. E., Rieke, G. H., Holmes, E., Lawler, S., Stapelfeldt, K. R., Werner, M. W., Gautier, T. N., III, Blaylock, M., et al. (2006) · The Astrophysical Journal · doi:10.1086/498093 · Cited by 264
Steady State Evolution of Debris Disks around A Stars
Wyatt, M. C., Smith, R., Su, K. Y. L., Rieke, G. H., Greaves, J. S., Beichman, C., & Bryden, G. (2007) · The Astrophysical Journal · doi:10.1086/518404 · Cited by 252
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Metadata
- 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 › 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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