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SpS5 - III. Matter ejection and feedback

Published online by Cambridge University Press:  05 March 2015

Yaël Nazé
Affiliation:
Department AGO, Allée du 6 Août 17, B5C, 4000-Liège, Belgium, email: naze@astro.ulg.ac.be
Xiao Che
Affiliation:
Dpt of Astronomy, Univ. of Michigan, 830 Dennison Bldg, Ann Arbor, MI 48109-1042, USA
Nick L. J. Cox
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, Leuven, Belgium
José H. Groh
Affiliation:
Geneva Observ., Univ. of Geneva, Chemin des Maillettes 51, CH-1290 Sauverny, Switzerland
Martin Guerrero
Affiliation:
IAA-CSIC, Glorieta de la Astronomia s/n, 18008 Granada, Spain
Pierre Kervella
Affiliation:
LESIA, Obs. de Paris, CNRS UMR 8109, UPMC, 5 place J. Janssen, 92195, Meudon, France
Chien-De Lee
Affiliation:
Graduate institute of astronomy, National central university, Taiwan
Mikako Matsuura
Affiliation:
Department of Physics and Astronomy, UCL, Gower Street, London WC1E 6BT, UK
M. Sally Oey
Affiliation:
Dpt of Astronomy, Univ. of Michigan, 830 Dennison Bldg, Ann Arbor, MI 48109-1042, USA
Guy S. Stringfellow
Affiliation:
Center for Astroph. and Space Astr., Univ. of Colorado, 389 UCB, Boulder, CO, USA
Stephanie Wachter
Affiliation:
IPAC, California Inst. of Technology, Pasadena, CA 91125, USA
Corresponding
E-mail address:
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Abstract

The last part of SpS5 dealt with the circumstellar environment. Structures are indeed found around several types of massive stars, such as blue and red supergiants, as well as WRs and LBVs. As shown in the last years, the potential of IR for their study is twofold: first, IR can help discover many previously unknown nebulae, leading to the identification of new massive stars as their progenitors; second, IR can help characterize the nebular features. Current and new IR facilities thus pave the way to a better understanding of the feedback from massive stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

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