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The End: Witnessing the Death of Extreme Carbon Stars

Published online by Cambridge University Press:  30 December 2019

G. C. Sloan Open the ORCID record for G. C. Sloan [Opens in a new window] ,
K. E. Kraemer ,
I. McDonald  and
A. A. Zijlstra Open the ORCID record for A. A. Zijlstra [Opens in a new window]
G. C. Sloan
Affiliation:
Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21248, USA email: sloan@astro.cornell.edu Univ. of North Carolina Chapel Hill, Chapel Hill, NC 27599-3255, USA
K. E. Kraemer
Affiliation:
Boston College, Chestnut Hill, MA 02467, USA
I. McDonald
Affiliation:
Jodrell Bank Centre for Astrophysics, Alan Turing Building, Manchester, M13 9PL, UK
A. A. Zijlstra
Affiliation:
Jodrell Bank Centre for Astrophysics, Alan Turing Building, Manchester, M13 9PL, UK
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Abstract

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A Last affiliation changed 3 to 4 against MS. Please check and confirm if it is fine. small number of the sample of 184 carbon stars in the Magellanic Clouds show signs that they are in the act of evolving off of the asymptotic giant branch. Most carbon stars grow progressively redder in all infrared colors and develop stronger pulsation amplitudes as their circumstellar dust shells become optically thicker. The reddest sources, however, have unexpectedly low pulsation amplitudes, and some even show blue excesses that could point to deviations from spherical symmetry as they eject the last of their envelopes. Previously, all dusty carbon-rich AGB stars have been labeled “extreme,” but that term should be reserved for the truly extreme carbon stars. These objects may well hold the clues needed to disentangle what actually happens when a star ejects the last of its envelope and evolves off of the AGB.

Keywords

infrared: starsstars: carbon stars: AGB and post-AGBMagellanic Clouds
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. 305 - 308
Copyright
© International Astronomical Union 2019 

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