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Session 45 - Eclipsing Binaries.
Display session, Thursday, January 08
Exhibit Hall,
iEO Aurigae was discovered to be an eclipsing binary with a 4.07 day period by S. Gaposchkin (1943) and was originally assumed from the spectroscopic analysis of Pearce (1943) to have two almost-identical, high-mass B3 III components. Popper (1978) indicated that the spectra showed the components to be less-massive O9 and B3 stars. Previous analyses of available light curves by Ramella et al. (1980) and Hartigan (1981) show marked disagreements in the values of the photometric elements. As a part of our long-term program to obtain modern light curves of interesting double-lined binary systems, we have observed EO Aurigae for the past three observing seasons on the 0.4 meter telescope at the Baker Observatory of SW Missouri State University. New light curves in the Cousins BVRI passbands have been obtained with our Photometrics CCD system, and a new model for EO Aurigae has been determined using the Wilson-Devinney program. This research has been supported by NSF grants AST-9315061 and AST-9605822 and NASA grant NGT-40029.
