Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-19T06:33:45.218Z Has data issue: false hasContentIssue false
  • English
  • Français

Michelson-Spectro-Interferometry (MSI) of Be stars envelopes with the GI2T Interferometer

Published online by Cambridge University Press:  12 April 2016

Ph. Stee ,
D. Bonneau ,
P. Lawson ,
F. Morand ,
D. Mourard ,
I. Tallon  and
F. Vakili
Ph. Stee
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
D. Bonneau
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
P. Lawson
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
F. Morand
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
D. Mourard
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
I. Tallon
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France
F. Vakili
Affiliation:
Observatoire de la Côte d’Azur 2130 route de l’Observatoire, Caussols 06460 St Vallier de Thiey, France

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.

The GI2T is an optical long-baseline Michelson interferometer which analyses dispersed stellar fringes in the multi-speckle mode with a spectral resolution of one Angstrom while the spatial resolution is about one milliarcsecond. This makes the GI2T a powerful instrument able to perform MSI of extended sources like Be stars or shell stars. In order to interpret these data we have developed a latitude dependent radiative wind model for Be stars. This numerical code enables us to compare directly computed 2D maps in some Balmer lines (Hα and Hβ) with high angular resolution data of some Be stars.

Type
5. Miscellaneous Methods
Information
International Astronomical Union Colloquium , Volume 149: Tridimensional Optical Spectroscopic Methods in Astrophysics , 1995 , pp. 365 - 368
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

Araújo, F.X., Freitas Pacheco, J.A. 1989, MNRAS, 241, 543 Google Scholar
Araújo, F.X., Freitas Pacheco, J.A., Petrini, D. 1993, MNRAS, 267, 501 Google Scholar
Friend, D.B., Abbott, D.C. 1986, ApJ, 311, 701 Google Scholar
Mourard, D., Bose, I., Blazit, A., Bonneau, D., Merlin, G., Morand, F., Vakili, F., Labeyrie, A. 1994, A&A, 283, 705 Google Scholar
Stee, Ph. and Araújo, F.X. 1994, A&A, in pressGoogle Scholar