[33.06] Emission from the Secondary Star in the CO Orionis Binary System

AAS 203rd Meeting, January 2004
Session 33 Young Stars
Oral, Monday, January 5, 2004, 2:00-3:30pm, Regency VII

[33.06] Emission from the Secondary Star in the CO Orionis Binary System

B. M. Rodgers (Gemini Observatory), L. M. Pierpoint (University of California Los Angeles), N. S. van der Bliek (Cerro Tololo International Observatory)

CO Orionis is a binary star system. The primary star is a late F or early G star and is generally considered to be a pre-main sequence star based on its apparent proximity to the Orionis star formation region and hydrogen emission lines (typically associated with accretion in young stars) observed in the system. The primary star is optically variable (delta-V ~ 3magnitudes) and therefore CO Ori is often included among "UXOR" type stars. We show spatially resolved Pa-beta and Br-gamma spectra from the system that clearly show the hydrogen emission is associated with the secondary star in the system, CO Ori B, not CO Ori A. We also present BVRIJHK photometry of each star, and discuss the possible nature of each component based on these data. Please see also the poster by L. Pierpoint & B. Rodgers on this topic.

The author(s) of this abstract have provided an email address for comments about the abstract: brodgers@gemini.edu

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