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A Possible Solution to the Mass-Loss Problem in M-type AGB Stars
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics.
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2011 (English)In: Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants, 2011, Vol. 445Conference paper (Refereed)
Abstract [en]

Mass loss is a fundamental, observationally well-established feature of AGB stars, but many aspects of this process are not yet understood. To date, self-consistent dynamical models of dust-driven winds reproducing the observed mass-loss rates seem only possible for M-type stars if the grains in the close circumstellar environment grow to larger sizes than previously assumed. In order to study the grain-size distribution where the mass loss is initiated, high-spatial-resolution interferometry observations are necessary. We have observed two M-type stars using the VLTI/MIDI instrument to constrain the dust-grain sizes through modeling the 10 μm silicate feature. Here we present preliminary results.

Place, publisher, year, edition, pages
2011. Vol. 445
, Astronomical Society of the Pacific Conference Series
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-170175OAI: oai:DiVA.org:uu-170175DiVA: diva2:508578
Astronomical Society of the Pacific Conference Series, 445
Available from: 2012-03-09 Created: 2012-03-09 Last updated: 2013-03-13

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Sacuto, StéphaneHöfner, Susanne
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