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Stellar Astrophysics with Sub-Milliarcsecond Optical Interferometry

Published online by Cambridge University Press:  07 August 2017

Ph. Stee
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
D. Bonneau
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
D. Mourard
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
P. Lawson
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
F. Morand
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
I. Tallon
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]
F. Vakili
Affiliation:
Equipe GI2T Observatoire de la Côte d'Azur 2130 route de l'Observatoire, Caussols, 06460 St Vallier de Thiey, France. email: [email protected]

Extract

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Although stellar interferometers are capable of measuring the angular diameters of stars, with longer baselines they may also be used to measure brightness variations across a star's surface and to provide constraints on models of stellar envelopes. In this paper we will look at the interpretation of visibility data and some of the more exciting prospects within the reach of current interferometers.

Type
2. Current and Future Needs for Very Accurate Astrometry
Copyright
Copyright © Kluwer 1995 

References

Araújo, F.X., & Freitas Pacheco, J.A., 1989, MNRAS, 241, 543.Google Scholar
Araújo, F.X., Freitas Pacheco, J.A., & Petrini, D., 1994, MNRAS, 267, 501 Google Scholar
Di Benedetto, P., & Foy, R., 1986, A&A, 166 , 204.Google Scholar
Di Benedetto, P., & Bonneau, D., 1990, ApJ, 358, 617.Google Scholar
Dupree, A.K., Baliunas, S.L., & Guinan, E.F., 1984, Workshop on High Angular Resolution Optical Interferometry , BAAS, 16, 797.Google Scholar
Friend, D.B., Abbott, D.C. 1986, ApJ, 311, 701 Google Scholar
Hanbury Brown, R., Davis, J., Lake, R. J. W., & Thomson, R. J., 1974, MNRAS, 167, 475.Google Scholar
Hummel, C.A., Armstrong, J.T., Quirrenbach, A., Buscher, D.F., Mozurkewich, D., Elias, N.M. II, & Wilson, R.E., 1994, AJ, 107, 1859.CrossRefGoogle Scholar
Schwarzchild, M., 1974, ApJ, 195, 137.Google Scholar
Stee, Ph., & Araújo, F.X., 1994, A&A, in press.Google Scholar
Stee, Ph., Araújo, F.X., Vakili, F., Mourard, D., Arnold, L., Bonneau, D., Morand, F. and Tallon-Bosc, I. 1994, A&A, submitted.Google Scholar
Vakili, F., Mourard, D., & Stee, Ph., 1994, IAU Symp. 162 on Pulsation, Rotation and Mass Loss in Early Type Stars, (Kluwer: Holland, 1994), pp. 435 Google Scholar