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Binary interactions on the RGB: Dusty post-RGB stars

Published online by Cambridge University Press:  08 August 2017

Devika Kamath ,
Hans Van Winckel  and
Peter Wood
Devika Kamath
Affiliation:
Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200D bus 2401, B-3001 Leuven, Belgium email: devika@ster.kuleuven.be
Hans Van Winckel
Affiliation:
Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200D bus 2401, B-3001 Leuven, Belgium email: devika@ster.kuleuven.be
Peter Wood
Affiliation:
Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Weston Creek, ACT 2611, Australia email: wood@mso.anu.edu.au
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Abstract

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It is widely accepted that binary interactions are responsible for the shaping of planetary nebula. However, these binary interactions and evolutionary channels are poorly understood. Our recent study revealed a newly discovered population of low-luminosity, low-metallicity, likely binaries in the Magellanic Clouds: dusty post-RGB stars. They are likely to have evolved off the RGB via binary interaction. In this paper we present preliminary results of the first radial velocity monitoring of the post-RGB stars in the Small Magellanic Cloud (SMC) and the implications on stellar (binary) evolution. We also investigate their link, if any, to the planetary nebulae systems.

Keywords

techniques: radial velocitiesstars: AGB and post-AGB(stars:) binaries: generalstars: evolutionstars: Population II(ISM:) planetary nebulae: generalGalaxy: general(galaxies:) Magellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 223 - 226
Copyright
Copyright © International Astronomical Union 2017 

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