Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-12T09:28:47.112Z Has data issue: false hasContentIssue false
  • English
  • Français

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 ,
H.J.G.L.M. Lamers  and
M. Perinotto
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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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
Information
Symposium - International Astronomical Union , Volume 122: Circumstellar Matter , 1987 , pp. 431 - 432
Copyright
Copyright © Reidel 1987 

References

Castor, J.I. and Lamers, H.J.G.L.M.; 1979, Astrophys. J. Suppl. 39, 481.Google 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