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The Structure of the Inner Circumstellar Shell in Miras

Published online by Cambridge University Press:  30 December 2019

Kenneth H. Hinkle Open the ORCID record for Kenneth H. Hinkle [Opens in a new window]  and
Thomas Lebzelter Open the ORCID record for Thomas Lebzelter [Opens in a new window]
Kenneth H. Hinkle
Affiliation:
National Optical Astronomy Observatory, P.O. Box 26732, Tucson, Az, USA email: [email protected]
Thomas Lebzelter
Affiliation:
Dept. of Astrophysics, Univ. of Vienna, Vienna, Austria email: [email protected]
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Abstract

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We have measured CO line profiles in a time series of 42 high-resolution 1.6 − 2.5 μm spectra of R Cas. The low-excitation CO first overtone lines have a contribution from a ∼1000 K region. We show that this region undergoes a periodic changes on time scales many times longer than the photospheric pulsation. Comparison with interferometry and models suggests that the ∼1000 K region is at ∼2 R* and cospatial with the region of SiO masers and grain condensation. The CO lines are entirely in absorption requiring formation in a layer thin compared to the stellar diameter. The CO excitation temperature has been measured as low as 600 K suggesting that grains with a variety of compositions condense at ∼2 R*.

Keywords

stars: AGB and post-AGB(stars:) circumstellar matterstars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 419 - 420
Copyright
© International Astronomical Union 2019 

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