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On the Nature of M stars with a 60 microns Excess

  • C. Loup (a1), L.B.F.M. Waters (a2), F. Kerschbaum (a3), J. Hron (a3), E. Josselin (a1), D. Kester (a4), Tj.R. Bontekoe (a4) and A. Zijlstra (a5)...

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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.

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References

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Bontekoe, Tj.R., Koper, E., & Rester, D.J.M. 1994, A&A 284, 1037
Chan, & S., Kwok 1988, ApJ, 334, 362
Olofsson, H., Carlström, U., Eriksson, K., & Gustafsson, B. 1992, A&A 253, L17
van der Veen, W.E.C.J, & Habing, H.J. 1988, A&A, 194, 125
Vassiliadis, E., & Wood, P.R. 1993, ApJ, 413, 641
Waters, L.B.F.M., et al. 1994, A&A, 281, L1
Willems, F.J., & de Jong, T. 1988, A&A, 196, 173
Zijlstra, A.A., Loup, C., Waters, L.B.F.M., & de Jong, T. 1992, A&A, 265, L5

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On the Nature of M stars with a 60 microns Excess

  • C. Loup (a1), L.B.F.M. Waters (a2), F. Kerschbaum (a3), J. Hron (a3), E. Josselin (a1), D. Kester (a4), Tj.R. Bontekoe (a4) and A. Zijlstra (a5)...

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