AAS 203rd Meeting, January 2004
Session 12 Eclipsing Binary Stars
Poster, Monday, January 5, 2004, 9:20am-6:30pm, Grand Hall

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[12.12] The secondary star of CO Orionis

L. Pierpoint (University of California, Los Angeles), B. Rodgers (Cerro Tololo Inter-American Observatory)

Abstract: While the system CO Orionis is often mentioned in explorations of young T-Tauri/HAEBE stars, its binary nature is usually overlooked. We use photometric data from the Blanco 4m telescope to determine individual characteristics of the primary and especially the secondary star. We calculate magnitudes in B,V,R and I filters and construct color-color diagrams. We hope eventually to compare these investigations to spectral data and spectral energy density (SED) diagrams. As ever more young star systems are shown to be binary, it is increasingly important to analyze the complex characteristics of what may prove to be a "typical" system. Thus we may validate or question current interpretations of HAEBE SED's and associated disk models. Preliminary magnitudes and colors for CO Ori show that the secondary star is SLIGHTLY redder than the primary star, and that both stars vary in magnitude somewhat over our data timescale of 4 days. The undergraduate contribution to this project is funded by the NSF through the Cerro Tololo Inter-American Observatory REU program.

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.