Abstract
Vega-like stars are infrared excess stars either nearing or already on the main sequence. The infrared excess is interpreted as evidence for the presence of extended dusty disks surrounding the stars. In a few cases, the disks have been directly imaged. While most of the disks are difficult to observe at optical and near-infrared wavelengths, a few disks are bright enough to study at 10 microns. Mid-infrared spectra from several of these mid-infrared bright Vega-like stars reveals a range of silicate emission features. Such features arise from the thermal emission of silicate grains in the disks. In some cases, the silicate features seen are similar to those seen towards some solar-system comets and interplanetary dust particles.
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© 1999 Springer Science+Business Media Dordrecht
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Butner, H.M., Walker, H.J., Wooden, D.H. (1999). The Dust Around Vega-Like Stars: A Bridge from Ysos to Comets. In: Greenberg, J.M., Li, A. (eds) Formation and Evolution of Solids in Space. NATO ASI Series, vol 523. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4806-1_29
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DOI: https://doi.org/10.1007/978-94-011-4806-1_29
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