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Dust in debris disk: Observations and laboratory experiments

Published online by Cambridge University Press:  12 October 2020

Johan Olofsson Open the ORCID record for Johan Olofsson [Opens in a new window]
Johan Olofsson*
Affiliation:
Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Playa Ancha, Valparaíso, Chile email: johan.olofsson@uv.cl Núcleo Milenio Formación Planetaria - NPF, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile
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Abstract

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Debris disks are the natural by-products of the star and planet formation processes. Since the 1980’s several thousands of debris disks have been detected, and the presence of a disk is inferred by the detection of excess emission over the photospheric emission. This thermal emission arises from (micron-sized or slightly bigger) dust grains heated by the central star. However, in the vast majority of cases, these observations are not spatially resolving the radial distribution of the dust, resulting in strong degeneracies in the modeling approach (radial distance vs minimum grain size mostly). Therefore the properties of the small dust grains remained largely unconstrained until the arrival of high angular resolution instruments, especially at optical and near-infrared wavelengths. In these proceeding some of the main results are presented that have been obtained over the past few years on the properties of small dust grains in debris disks, and it is discussed how laboratory experiments contributed to put those results in context.

Keywords

stars: circumstellar mattertechniques: high angular resolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 169 - 175
Copyright
© International Astronomical Union 2020

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