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A method for calculation of line profiles in expanding atmospheres: Application to winds from central stars of planetary nebulae

Published online by Cambridge University Press:  04 August 2017

M. Cerruti-Sola
Affiliation:
1) Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 - 50125 Firenze, Italy
H.J.G.L.M. Lamers
Affiliation:
2) SRON Laboratory for Space Research Beneluxlaan 21, 3527 HS, Utrecht, The Netherlands
M. Perinotto
Affiliation:
3) Istituto di Astronomia, Università di Firenze Largo Enrico Fermi 5, 50125 Firenze, Italy

Extract

The structure of a stellar wind and its associated mass loss can be derived from the analysis of ñ Cygni-like line profiles. These do better occur in the UV range and have been extensively observed with the Copernicus (900–1450 A) and IUE Satellites (1150–3200 A).

Type
Mass Loss from Hot Stars
Copyright
Copyright © Reidel 1987 

References

Castor, J.I. and Lamers, H.J.G.L.M.; 1979, Astrophys. J. Suppl. 39, 481.CrossRefGoogle Scholar
Hamann, W.-R.: 1980, Astron. Astrophys. 84, 342.Google Scholar
Hamann, W.-R.: 1981, Astron. Astrophys. 93, 353.Google Scholar
Mihalas, D., Kunasz, P.B. Hummer, D.G.: 1975, Astrophys. J. 202, 465.CrossRefGoogle Scholar

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