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Mass Loss from Stars

Published online by Cambridge University Press:  14 August 2015

S. R. Pottasch
S. R. Pottasch*
Affiliation:
Sterrekundig Laboratorium Kapteijn, Groningen, The Netherlands

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In this summary we shall attempt to evaluate the mass loss from several kinds of high luminosity stars, especially planetary nebulae, OB supergiants and M giants and supergiants. The purpose is to give an observational basis for the discussion of the mechanism of mass loss and of the consequences of stellar mass loss for the interstellar medium and for stellar evolution. For reasons which will presently be discussed, we are now certain that mass loss is occurring in all the objects mentioned, and probably to a similar extent in all high luminosity stars as well. The precise values of the mass loss rate are uncertain at present; for some objects the uncertainty will be large (two orders of magnitude) and have important influence on the consequences of the mass loss. Therefore we shall discuss in some detail how the different loss rates quoted in the literature have been obtained and what assumptions have been made (see also the Report by Boyarchuk, p. 281). On the basis of this discussion we will indicate the most probable loss rates and their consequences, always remembering the possible influence of the uncertainties.

Type
Part II: Interaction of Stars and Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 39: Interstellar Gas Dynamics , 1970 , pp. 272 - 280
Copyright
Copyright © Reidel 1970 

References

Allen, C. W.: 1963, Astrophysical Quantities, Athlone Press, London.Google Scholar
Aller, L. H. and Liller, W.: 1968, in Nebulae and Interstellar Matter (ed. by Aller, L. H. and Middlehurst, B.), University of Chicago Press, Chicago, p. 483.Google Scholar
Biermann, L.: 1951, Z. Astrophys. 29, 274.Google Scholar
Blanco, V. M.: 1965, in Galactic Structure (ed. by Blaauw, A. and Schmidt, M.), University of Chicago Press, Chicago, p. 241.Google Scholar
Cahn, J. H.: 1968, in IAU Symposium No. 34, Planetary Nebulae (ed. by Osterbrock, D. E. and O'Dell, C. R.), Reidel, Dordrecht, The Netherlands, p. 44.Google Scholar
Deutsch, A. J.: 1956, Astrophys. J. 123, 210.Google Scholar
Deutsch, A. J.: 1960, in Stellar Atmospheres (ed. by Greenstein, J. L.), University of Chicago Press, Chicago, p. 543.Google Scholar
De Groot, M.: 1969, Bull. Astron. Inst. Netherl. 20, 225.Google Scholar
Hutchings, J. B.: 1968, Monthly Notices Roy. Astron. Soc. 141, 219; 141, 329.Google Scholar
Hutchings, J. B.: 1969a, Monthly Notices Roy Astron. Soc. 144, 235.Google Scholar
Hutchings, J. B.: 1969b, preprints.Google Scholar
Morton, D. C.: 1967, Astrophys. J. 150, 535.Google Scholar
Neckel, H.: 1958, Astrophys. J. 128, 510.CrossRefGoogle Scholar
Ness, N. F.: 1968, Ann. Rev. Astron. Astrophys. 6, 79.Google Scholar
O'Dell, C. R.: 1968, in IAU Symposium No. 34, Planetary Nebulae (ed. by Osterbrock, D. E. and O'Dell, C. R.), Reidel, Dordrecht, The Netherlands, p. 361.Google Scholar
Sharpless, S.: 1965, in Galactic Structure (ed. by Blaauw, A. and Schmidt, M.), University of Chicago Press, Chicago.Google Scholar
Spitzer, L. Jr.: 1968, in Nebulae and Interstellar Matter (ed. by Aller, L. H. and Middlehurst, B.) University of Chicago Press, Chicago, p. 1.Google Scholar
Weymann, R.: 1962, Astrophys. J. 136, 844.CrossRefGoogle Scholar