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Modelling Stellar Rotation for Optical Long Baseline Interferometry

Published online by Cambridge University Press:  26 May 2016

A. Domiciano de Souza ,
J. Zorec ,
S. Jankov ,
F. Vakili  and
L. Abe
A. Domiciano de Souza
Affiliation:
Département d'Astrophysique de l'Université de Nice/Sophia-Antipolis, CNRS UMR 6525, France
J. Zorec
Affiliation:
Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, F-75014 Paris, France
S. Jankov
Affiliation:
Département d'Astrophysique de l'Université de Nice/Sophia-Antipolis, CNRS UMR 6525, France
F. Vakili
Affiliation:
Département d'Astrophysique de l'Université de Nice/Sophia-Antipolis, CNRS UMR 6525, France
L. Abe
Affiliation:
Département d'Astrophysique de l'Université de Nice/Sophia-Antipolis, CNRS UMR 6525, France

Abstract

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Optical long baseline interferometry is a technique sensitive to sky projected brightness distributions, constituting a powerful tool for the study of detailed stellar surface structures. Moreover, by combining high spectral and angular resolution we obtain a technique called differential interferometry that is also sensitive to mechanisms that induce chromatic signatures, such as stellar spots and large scale mass motions (e.g. rapid rotation, non-radial pulsations, shear currents produced by hydrodynamical instabilities). We present here a study of the signatures of stellar rotation on differential interferometry observables showing that they are very sensitive to differential rotation and stellar inclination.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 187 - 188
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Domiciano de Souza, A. et al. 2002, A&A 393, 345 Google Scholar
Reiners, & Schmitt, 2002, A&A 384, 155 Google Scholar