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IRAS Observations of Symbiotic Stars

Published online by Cambridge University Press:  12 April 2016

M. Parthasarathy
Affiliation:
Indian Institute of Astrophysics, Bangalore - 560034, India
H.C. Bhatt
Affiliation:
Indian Institute of Astrophysics, Bangalore - 560034, India

Abstract

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Of the 129 symbiotic stars in Allen's (1984) catalogue, 42 were found to be IRAS sources. Of these 42 IRAS sources, 22 are D-type (symbiotic Miras), 5 are D'-type (yellow symbiotics) and 15 are S-type. The separation of S, D and D’ types into three distinct groups is clearer in the log[fλ(25μm)/fλ(12μm)] versus (H-K) diagram. The IRAS fluxes of S-type symbiotics are consistent with that observed from normal M giants. This result suggests that mass-loss rate from most of the S-type symbiotics is similar to that from normal M giants. The IRAS data of D-type symbiotics shows evidence for the presence of dust envelopes. The masses of the dust envelopes (10-6 to 10-7 Mo) around Miras in D-type symbiotics are similar to that observed in field Mira variables. These results suggest that mass-loss rates in symbiotic Miras are similar to those from field Mira variables and also that the mass loss from symbiotic Miras is pulsationally driven similar to that found in field Mira variables by Whitelock, Pottasch and Feast (1987). Analysis of IRAS data of yellow symbiotics Ml-2, AS201, Cnl-1, Wray 157. and HD149427 suggests that they are young planetary nebulae containing a binary nucleus. Ml-2, AS201 and Cnl-1 show evidence for the presence of evolved hot companions. The evolutionary stage of the late type (F-G) companions is not clear.

Type
5. Chromospheres, Winds and Mass Loss
Copyright
Copyright © Cambridge University Press 1989

References

Allen, D.A. 1982, In The Nature of Symbiotic Stars IAU Colloquium No. 70, ed. Friedjung, M. and Viotti, R. (Dordrecht: Reidei), p. 27.CrossRefGoogle Scholar
Allen, D.A. 1984, Proc. Astron. Soc. Australia. 5, 369.Google Scholar
Beichman, CA., Neugebauer, G., Habing, H.J., Clegg, P.E., and Chester, T.J. 1985, IRAS Point Source Catalogue, JPL.Google Scholar
Bhatt, H.C., Mallik, D.C.V. 1986, Astron. Astrophvs. 168, 248.Google Scholar
Draine, B.T., Lee, H.M. 1984, Astrophvs. J. 285, 89.Google Scholar
Feast, M.W. 1984, Mon. Not. R. Astr. Soc. 211, 51p.Google Scholar
Feibelman, W.A. 1983, Astrophvs. J, 275, 628.Google Scholar
Feibelman, W.A. 1988, in A Decade of UV Astronomy with IUE. ESA SP-281, p. 179.Google Scholar
Glass, I.S., Webster, B.L. 1973, Mon. Not. R. Astr. Soc. 165, 77.Google Scholar
Gutierrez-Moreno, A. et al. 1987, Preprint Dept. Astro. Univ. Chile. Google Scholar
Hilderbrand, R.H. 1983, Quart, i. Roy. Astron. Soc. 24, 267.Google Scholar
Kenyon, S.J., Fernandez-Castro, T., Stencel, R.F. 1986. Astron. J. 92, 1118.Google Scholar
Kenyon, S.J., Gallagher, J.S. 1983. Astron. J. 88, 666.Google Scholar
Kenyon, S.J., Webbink, R.F. 1984, Astrophvs. J. 279. 252.Google Scholar
Kohoutek, L. 1977. in Planetary Nebulae (IAU Symp. 76) ed. Terzian, Y. (Dordrecht: Reidel). p. 47.Google Scholar
Kohoutek, L. 1987, Astrophvs. and Space Science 131, 781.CrossRefGoogle Scholar
Lutz, J.H. 1984, Astrophvs. J. 279. 714.Google Scholar
O'Dell, C.R. 1966, Astrophvs. J. 145, 487.Google Scholar
Olnon, F.M., Raimond, E. 1986. Astron. Astrophvs. Suppl. 65, 607.Google Scholar
Roche, P.F., Allen, D.A., Aitken, D.K. 1983, Mon. Not. IL. Astron. Soc. 204, 1009.Google Scholar
Webster, B.L., Allen, D.A. 1975, Mon. Not. R. Astro. Soc. 171, 171.CrossRefGoogle Scholar
Whitelock, P.A. 1987, Pubi. Astro. Soc. Pac. 99, 573.Google Scholar
Whitelock, P.A., Pottasch, S.R., Feast, M.W. 1987, in Late Stages of Stellar Evolution, ed. Kwok, S. and Pottasch, S.R. (Dordrecht: Reidel), p. 269.CrossRefGoogle Scholar