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arXiv 1306.6647astro-ph.SR
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御夫座V582 F或F星的光度和光谱变化

Photometric and spectroscopic variability of the FUor star V582 Aurigae

E. H. Semkov, S. P. Peneva, U. Munari, M. Dennefeld, H. Mito, D. P. Dimitrov, S. Ibryamov, K. A. Stoyanov

备注：
9 pages, 8 figures, accepted for publication in A&A
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摘要：

2009年8月至2013年2月，我们在V582 Aur野外进行了BVRI CCD测光观测。在此期间，我们获得了V582 Aur的高，中，低分辨率光谱。为了研究目标爆发前的变化并构建其历史光变曲线，我们在照相底片收藏中搜索了存档观测。CCD和摄影观测进行了分析，使用一个序列的14颗恒星的领域V582 Aur在BVRI校准。V582 Aur爆发前的摄影观测显示出金牛T星典型的低振幅光变化。档案摄影观测表明，这颗恒星的亮度在1984年底或1985年初开始增加，并在1986年1月达到最大亮度。V582 Aur的光谱类型可以定义为G 0 I，具有H α和Na I D线的强P Cyg轮廓，这是典型的FU Orionis天体。我们的BVRI光度观测表明，在3.5年的观测期间，大幅度变化V~2.8等。然而，大多数时候，恒星保持在接近最大亮度的状态。亮度下降最深的一次是在2012年春天，当时恒星的亮度下降到接近爆发前的水平。在最小亮度期间，太阳光度数据显示颜色反转，这是UX Ori变星的典型特征。相应的光谱观测表明，谱线（特别是H α）的轮廓和强度具有很强的可变性，这表明吸积速率发生了显着变化。在过去三年进行的光度监测的基础上，最大光的光谱特性和长期光变曲线的形状，我们确认了V582 Aur与FU Orionis天体组的联系。

英文摘要：

We carried out BVRI CCD photometric observations in the field of V582 Aur from 2009 August to 2013 February. We acquired high-, medium-, and low-resolution spectroscopy of V582 Aur during this period. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using a sequence of 14 stars in the field of V582 Aur calibrated in BVRI. The pre-outburst photographic observations of V582 Aur show low-amplitude light variations typical of T Tauri stars. Archival photographic observations indicate that the increase in brightness began in late 1984 or early 1985 and the star reached the maximum level of brightness at 1986 January. The spectral type of V582 Aur can be defined as G0I with strong P Cyg profiles of H alpha and Na I D lines, which are typical of FU Orionis objects. Our BVRI photometric observations show large amplitude variations V~2.8 mag. during the 3.5 year period of observations. Most of the time, however, the star remains in a state close to the maximum brightness. The deepest drop in brightness was observed in the spring of 2012, when the brightness of the star fell to a level close to the pre-outburst. The multicolor photometric data show a color reversal during the minimum in brightness, which is typical of UX Ori variables. The corresponding spectral observations show strong variability in the profiles and intensities of the spectral lines (especially H alpha), which indicate significant changes in the accretion rate. On the basis of photometric monitoring performed over the past three years, the spectral properties of the maximal light, and the shape of the long-term light curve, we confirm the affiliation of V582 Aur to the group of FU Orionis objects.

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