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On the Nature of M stars with a 60 microns Excess

Published online by Cambridge University Press:  12 April 2016

C. Loup ,
L.B.F.M. Waters ,
F. Kerschbaum ,
J. Hron ,
E. Josselin ,
D. Kester ,
Tj.R. Bontekoe  and
A. Zijlstra
C. Loup
Affiliation:
Institut d’Astrophysique de Paris, CNRS, France
L.B.F.M. Waters
Affiliation:
Astronomical Institute Anton Pannekoek, Amsterdam, the Netherlands
F. Kerschbaum
Affiliation:
Institut für Astronomie, Wien, Austria
J. Hron
Affiliation:
Institut für Astronomie, Wien, Austria
E. Josselin
Affiliation:
Institut d’Astrophysique de Paris, CNRS, France
D. Kester
Affiliation:
SRON Space Research Laboratory, Groningen, the Netherlands
Tj.R. Bontekoe
Affiliation:
SRON Space Research Laboratory, Groningen, the Netherlands
A. Zijlstra
Affiliation:
European Southern Observatory, Garching, Germany

Extract

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Some years ago, Willems & de Jong (1988) noticed that many carbon stars display an excess of emission at 60 µm and explained it by the presence of a fossil dust shell, containing only cold dust. This detached dust shell would be the result of an interruption of the mass loss, consequence of a thermal pulse. Detached shells around C stars have actually been mapped in the CO lines (Olofsson et al. 1992), and at 60µm (Waters et al. 1994). In 1992, Zijlstra et al. found about 100 M stars displaying an excess of emission at 60 µm, and proposed that interruptions of the mass loss due to thermal pulses is a general phenomenon on the AGB. This assumption is now supported by the theoretical calculations of Vassiliadis & Wood (1993). Here we present a detailed study of the 100 M stars of Zijlstra et al. in order to test the previous assumption.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 425 - 426
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

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