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Exploring dust mass and dust properties of nearby AGB stars

Published online by Cambridge University Press:  30 December 2019

J. Wiegert Open the ORCID record for J. Wiegert [Opens in a new window] ,
M. A. T. Groenewegen Open the ORCID record for M. A. T. Groenewegen [Opens in a new window]  and
the STARLAB team
J. Wiegert
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium email: [email protected]
M. A. T. Groenewegen
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium email: [email protected]
the STARLAB team
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

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Low and intermediate mass stars evolve to the asymptotic red giant branch (AGB) late in their lives. These are surrounded by a circumstellar envelope (CSE) filled with gas and dust. The dust is formed close to the star at sublimation radii and is pushed away by the stellar wind. The dust in turn pushes gases from the envelope into the interstellar medium, thus enriching it with metals. This poster summary is a general description of the next piece of a larger project, whereas the first half has been published by Nicolaes et al. (2018). We now aim to use radiative transfer simulations to model spectral energy distributions (SED) of dust and fit them to far-infrared observations for the same 40 sources. We will use 2D and 3D simulations and models containing several dust species simultaneously.

Keywords

stars: AGB and post-AGB(stars:) circumstellar matterstars: mass lossstars: windsoutflowsinfrared: starssubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 542 - 543
Copyright
© International Astronomical Union 2019 

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