Volume 411, Number 2, November IV 2003
|Page(s)||197 - 202|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
Two new bright Ae stars*
Physics & Astronomy Department, The University of Western Ontario, London, Ontario N6A 3K7, Canada
2 Special Astrophysical Observatory of Russian AS, Nizhnij Arkhyz 369167, Russia
3 Department of Physics, Royal Military College of Canada, Kingston, Ontario K7K 7B4, Canada
Corresponding author: D. N. Monin, email@example.com
Accepted: 28 July 2003
Two newly identified Ae stars, ν Cyg and κ UMa, were discovered in the course of the Magnetic Survey of Bright main sequence stars (Monin et al. 2002). We present their Hα profiles along with measurements of their equivalent width and parameters of emission features. Emission in the Hα line of ν Cyg is variable on a time scale of 3 years. κ UMa exhibits weak emission which is rather stable. The emission is thought to arise from a circumstellar disk, and we have estimated the size of that disk.Both new emission stars are IRAS sources. Their IR color excesses are consistent with those of classical Ae stars. Thus, ν Cyg and κ UMa appear not to belong to the class of Herbig Ae/Be stars. We argue that the frequency of Ae stars may be underestimated due to the difficulty of detection of weak emission in some A stars.
Key words: stars: emission line, Be / stars: individual: ν Cyg / stars: individual: κ UMa
© ESO, 2003
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