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Interferometric Observations of Mira Variables

Published online by Cambridge University Press:  26 May 2016

G. Van Belle ,
R. R. Thompson  and
M.J. Creech-Eakman
G. Van Belle
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
R. R. Thompson
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
M.J. Creech-Eakman
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109

Abstract

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Milliarcsecond resolution observations of cool stars are becoming increasingly common and sophisticated as recent advances in telescope technology mature. To varying degrees, these observations rely up on stellar models for interpretation of their data, while at the same time present particular challenges to those models. Indications of departures from spherical symmetry are beginning to be observed as increasingly rich image information is obtained by a new generation of interferometers. Examination the subtle variations of wavelength-specific sizes exhibits rich structure, connected to the atmospheric chemistry. For the pulsating stars, such as Mira variables, that structure varies with time, with the phase lags between the various sizes being connected to the atmospheric dynamics. Complex morphologies associated with atmospheric winds have been revealed with these high resolution experiments. A review of these recent results will be presented, concentrated on their implications upon stellar modelling, and the prospects for future observational data.

Type
Session F. Winds - Cool and Pulsating Stars
Information
Symposium - International Astronomical Union , Volume 210: Modelling of Stellar Atmospheres , 2003 , pp. 367 - 376
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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