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The evolution of DARWIN: current status of wind models for AGB stars

Published online by Cambridge University Press:  30 December 2019

Sara Bladh
Sara Bladh*
Affiliation:
Division of Astronomy and Space Physics, Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden email: sara.bladh@physics.uu.se
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Abstract

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The slow, dense winds observed in evolved asymptotic giant branch (AGB) stars are usually attributed to a combination of dust formation in the dynamical inner atmosphere of these stars and momentum transfer from stellar photons interacting with the newly formed dust particles. Wind models calculated with the DARWIN code, using this mass-loss scenario, have successfully produced outflows with dynamical and photometric properties compatible with observations, for both C-type and M-type AGB stars. Presented here is an overview of the DARWIN models currently available and what output these models produce, as well as future plans.

Keywords

stars: AGB and post-AGBstars: atmospheresstars: carbonstars: mass lossstars: windsoutflowsshock wavesstellar dynamics
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. 99 - 107
Copyright
© International Astronomical Union 2019 

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