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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 358642.0, MPI für Astronomie / Publikationen_mpia
Dust in protoplanetary disks: properties and evolution
Authors:Natta, A.; Testi, L.; Calvet, N.; Henning, Th; Waters, R.; Wilner, D.
Language:English
Place of Publication:Tucson
Publisher:University of Arizona Pr.
Date of Publication (YYYY-MM-DD):2007
Title of Book:Protostars and Planets V
Start Page:767
End Page:781
Full Name of Book-Editor(s):Reipurth, B.; Jewitt, J.; Keil, K.
Title of Series:The University of Arizona space science series
Review Status:not specified
Audience:Experts Only
Abstract / Description:We review the properties of dust in protoplanetary disks around optically visible pre-main-sequence stars obtained with a variety of observational techniques, from measurements of scattered light at visual and infrared wavelengths to mid-infrared spectroscopy and millimeter interferometry. A general result is that grains in disks are on average much larger than in the diffuse interstellar medium (ISM). In many disks, there is evidence that a large mass of dust is in grains with millimeter and centimeter sizes, more similar to "sand and pebbles" than to grains. Smaller grains (with micrometer sizes) exist closer to the disk surface, which also contains much smaller particles, e.g., polycyclic aromatic hydrocarbons. There is some evidence of a vertical stratification, with smaller grains closer to the surface. Another difference with ISM is the higher fraction of crystalline relative to amorphous silicates found in disk surfaces. There is a large scatter in dust properties among different sources, but no evidence of correlation with the stellar properties, for samples that include objects from intermediate to solar mass stars and brown dwarfs. There is also no apparent correlation with the age of the central object, over a range roughly between 1 and 10 m.y. This suggests a scenario in which significant grain processing may occur very early in the disk evolution, possibly when it is accreting matter from the parental molecular core. Further evolution may occur, but not necessarily rapidly, since we have evidence that large amounts of grains, from micrometer to centimeter size, can survive for periods as long as 10 m.y.
External Publication Status:published
Document Type:InBook
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISBN:0-8165-2654-0 [ID No:1]
URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi... [ID No:2]
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