Astronomy and Astrophysics – Astrophysics
Scientific paper
2001-01-03
Astronomy and Astrophysics
Astrophysics
7 pages, 5 figures, Accepted for publication in Ap&SS
Scientific paper
We present a series of optical spectroscopic and near-infrared photometric observations of the Be star X Persei, from the beginning of the recent emission phase. Our data show that after the latest extended low state (ELS), both the equivalent width (EW) of the H\alpha emission line and the JHK luminosities gradually increased. The recent maximum H\alpha EW and JHK magnitudes are more than but comparable to the 1986-1989 maxima, which reflects a more extensive and denser envelope in the new emission phase. The IR photometry and the H\alpha EW increase coincidently in the early stage of the new emission phase. However, the variations in the following years, specially in 1994 and 1995, are much different from the early variations. An unusual variation that while the H\alpha EW in X Per increases considerably, the JHK magnitudes decline rapidly is seen in our nearly simultaneous pectroscopic and near-infrared observations. An expanding ring model is put forward to interpret the observed unusual variations between the H\alpha EW and near-IR luminosity during the recent emission phase of X Persei. Our results indicate that although both infrared excess and H\alpha emission line arise from the envelope, their main ontributors, in some cases, are likely to originate in the different part of the envelope.
Hang Heng-Rong
Liu Zhi-Qiang
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