Hostname: page-component-848d4c4894-wg55d Total loading time: 0 Render date: 2024-06-09T09:34:33.400Z Has data issue: false hasContentIssue false
  • English
  • Français

High Resolution Interferometric Observations of Eclipsing Binary Stars

Published online by Cambridge University Press:  19 July 2016

Xiaopei Pan ,
Michael Shao  and
M. Mark Colavita
Xiaopei Pan
Affiliation:
California Institute of Technology, Pasadena, CA 91125
Michael Shao
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA 91109
M. Mark Colavita
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA 91109

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.

Eclipsing binary stars are of great importance in astronomy. Now, high angular resolution measurements of eclipsing stars with the Mark III Stellar Interferometer (Shao 1988) can determine not only all of the orbital parameters, but also the luminosities and color indices of the two components, and can yield precise information for the study of the stellar evolution models. Particularly, the combination of interferometric and photometric results provide a direct measurement of stellar effective temperature. In the case where the primary component can be resolved, the results from the optical interferometer then provide a reliable determination of the absolute system parameters. In addition, eclipsing binary stars are good candidates for comparison of different techniques, i.e., interferometric, photometric, astrometric, and spectroscopic, and for checking whether systematic uncertainties exist with certain techniques.

Type
Imaging Results: Optical and Infrared
Information
Symposium - International Astronomical Union , Volume 158: Very High Angular Resolution Imaging , 1994 , pp. 413 - 415
Copyright
Copyright © Kluwer 1994 

References

Pan, X. P., Shao, M., Colavita, M. M., Armstrong, J. T., Mozurkewich, D., Vivekanand, M., Denison, C. S., Simon, R. S., and Johnston, K. J. 1992, Ap. J., 384, 624.Google Scholar
Shao, M., Colavita, M. M., Hines, B. E., Staelin, D. H., Hutter, D. J., Johnston, K. J., Mozurkewich, D., Simon, R. S., Hershey, J. L., Hughes, J. A. and Kaplan, G. H. 1988, Astron. Astrophys., 193, 357.Google Scholar