Hostname: page-component-6bf8c574d5-n2sc8 Total loading time: 0 Render date: 2025-03-09T16:13:30.918Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic Field and Silicon diffusion in Bp-Si Stars

Published online by Cambridge University Press:  19 July 2016

C. Mégessier ,
T. Lanz  and
J. D. Landstreet
C. Mégessier
Affiliation:
Observatoire de Paris–Meudon, place J. Janssen 92195 Meudon France
T. Lanz
Affiliation:
Institut d'Astronomie de l'Université de Lausanne CH-1290 Chavannes-des-Bois, Switzerland
J. D. Landstreet
Affiliation:
Department of Astronomy University of Western Ontario London, Ontario, Canada N6A 3K7

Abstract

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.

SiII lines of magnetic Bp-Si stars in open clusters have been observed with the CAT (ESO) in order to get a mapping of the Silicon abundance distribution over the stellar surface, in the frame of the oblique rotator model. We point out the influence of the Zeeman splitting and of the abundance inhomogeneities on the line profiles.

Type
V. Magnetic Pieuds
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 329 - 332
Copyright
Copyright © Kluwer 1988 

References

Mégessier, C.: 1984, Astron. Astrophys. 138, 267 Google Scholar
Michaud, G., Mégessier, C., Charland, Y.: 1981, Astron. Astrophys. 103, 244 Google Scholar