[182.18] The $3\,\mu$m water ice/vapour feature of (post-)AGB stars

AAS 207th Meeting, 8-12 January 2006
Session 182 Stellar Winds, Circumstellar Matter, and Activity
Poster, Thursday, 9:20am-4:00pm, January 12, 2006, Exhibit Hall

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[182.18] The 3\,\mum water ice/vapour feature of (post-)AGB stars

C. Dijkstra (University of Missouri-Columbia), K. Justtanont (Stockholm Observatory), C. Dominik, L. B. F. M. Waters (University of Amsterdam), M. Matsuura (University of Manchester), A. K. Speck (University of Missouri-Columbia), J. Cami (NASA Ames Research Center), I. Yamamura (Laboratory of Infrared Astrophysics)

Asymptotic Giant Branch (AGB) stars are the highly evolved descendants of 1{\ }{\leq}{\ }M<8{\ }\rm{M_\odot} main sequence stars. They lose mass at a high rate, and through the so-called post-AGB phase evolve into planetary nebulae. The outflowing matter creates a dusty molecular circumstellar envelope, in which both water ice and water vapour may be present. The water ice and vapour may be studied using their near infrared 3\,\mum features. Current research on these features is discussed, with a particular emphasis on how they may be used to study the ice formation process and the structure of the ice formation region around (post-)AGB stars.

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