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Interpreting the Evolving Clumpy Shell Structure of IRC +10216 in Terms of Time Dependent Dust Shell Models

Published online by Cambridge University Press:  26 May 2016

J. M. Winters ,
T. Blöcker ,
K.-H. Hofmann  and
G. Weigelt
J. M. Winters
Affiliation:
Max-Planck Institut für Radioastronomie, D-53121 Bonn, Germany
T. Blöcker
Affiliation:
Max-Planck Institut für Radioastronomie, D-53121 Bonn, Germany
K.-H. Hofmann
Affiliation:
Max-Planck Institut für Radioastronomie, D-53121 Bonn, Germany
G. Weigelt
Affiliation:
Max-Planck Institut für Radioastronomie, D-53121 Bonn, Germany

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The prototypical dust-enshrouded carbon Mira IRC +10216 is known to exhibit intrinsic changes on a time scale of the order of only a few years as revealed, e.g., by CO infrared line profiles (Winters et al. 2000a), its infrared light curves, and by high spatial resolution monitoring in the infrared (Osterbart et al. 2000; Tuthill et al. 2000). In particular, the infrared light curves indicate a possible periodicity on a ≈ 20 yr time scale, i.e. that a recurrent phenomenon might lead to the observed variations. Such multi-periodicity time scales of several (≈ 10) stellar pulsation periods are predicted by consistent hydrodynamical models which include a proper treatment of dust formation (e.g. Winters et al. 2000b). In these models discrete dust layers form in time intervals which are several times longer than the typical pulsation period of an AGB star (Fleischer, Gauger, & Sedlmayr 1995; Höfner, Feuchtinger, & Dorfi 1995).

Type
Part III: Planetary Nebulae in the Scheme of Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 127 - 128
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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