arXiv 0812.10542008-12-05astro-ph

Be/X射线双星系统V0332 +53的长期光学观测

Long-term optical observations of Be/X-Ray binary system V0332+53

U. Kiziloglu, N. Kiziloglu, A. Baykal, S. K. Yerli, M. Ozbey

备注：: 4 pages, 2 figures
发表信息：: IBVS, 2008, No: 5865

摘要：

自2004年以来，我们一直在使用位于土耳其安塔利亚Bakirlitepe的45 cm ROTSEIIId望远镜和RTT 150（俄罗斯-土耳其1.5 m望远镜）监测双星系统V0332+53（光学对应物是BQ Cam）。我们报告这个系统的长期变化到目前为止。在MJD 53400之后的BQ Cam光中存在0.2 mag的衰减。BQ Cam的光变曲线的衰减可能是由于星周盘的密度或尺寸的减小。我们提供了Krimm等人（2008）报告的新X射线活动之前（在MJD 54730）和期间（在MJD 54768）获得的光谱观测。所观察到的Ha线轮廓是单峰的，几乎对称。发现目前的EW值与Negueruela等人（1999）在红外震级衰落期间观测到的EW值相似。发现Ha发射线红移约140 km/s，大于Corbet等人（1986）的发现。我们认为MJD 54700之后的盘变亮可能是由于盘的进动。

英文摘要：

We have been monitoring the binary system V0332+53 (optical counterpart is BQ Cam) since 2004 using 45 cm ROTSEIIId telescope and RTT150 (Russian-Turkish 1.5 m Telescope) located at Bakirlitepe, Antalya, Turkey. We report on the long-term variability of this system up to the present date. There exists a fading of 0.2 mag in the light of BQ Cam after MJD 53400. The fading in the light curve of BQ Cam could be due to a decrease in the density or in the size of the circumstellar disk. We present optical spectroscopic observations obtained before (at MJD 54730) and during (at MJD 54768) the new X-ray activity reported by Krimm et al. (2008). The observed Ha line profiles were single-peaked and almost symmetric. The present EW values are found to be similar to the ones observed during the fading of infrared magnitudes of Negueruela et al. (1999). Ha emission lines were found to be red-shifted by ~140 km/s which were larger than the findings of Corbet et al. (1986). We suggest that brightening of the disk after MJD 54700 may be due to the precession of the disk.

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