Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.3306r&link_type=abstract
American Astronomical Society Meeting 203, #33.06; Bulletin of the American Astronomical Society, Vol. 35, p.1257
Astronomy and Astrophysics
Astronomy
Scientific paper
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.
Pierpoint L. M.
Rodgers Bernadette Marie
van der Bliek Nicole S.
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