New findings supporting the presence of a thick disc and bipolar jets in the β Lyrae system
New findings supporting the presence of a thick disc and bipolar jets in the β Lyrae system
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新发现支持天琴座β系统中存在厚圆盘和双极喷流
DOI：
10.1051/0004-6361:20065536
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发表时间：
2007
影响因子：
6.5
通讯作者：
D. Sudar
中科院分区：
文献类型：
--
作者：
H. Ak;P. Chadima;P. Harmanec;O. Demircan;Shoufeng Yang;P. Koubský;P. Škoda;M. Šlechta;M. Wolf;H. Božić;D. Ruždjak;D. Sudar
上下文要了解双星中的大规模质量交换，还需要研究过程中快速阶段的复杂物体。β Lyr就是这样一个物体。目标。我们的目标是分析天琴座β星的52个照相光谱和651个电子光谱，以获得关于星周物质的更多信息，并首次研究分光光度信息。方法.用FOTEL程序进行轨道解算，得到改进的二次星历。使用KOREL程序解开光谱。15个较强的吸收线的主要分光光度的数量进行了测量和校正的轨道连续变化使用的流量计算从一个适合的光变曲线与BINSYN程序。测量H α发射线的V和R峰的中心强度，并使用程序PERIOD04数值模拟的R带光变曲线对轨道光变进行校正。结果解开的摄影和电子光谱导致检测到弱吸收线起源于吸积盘的伪光球。通过这种方式，获得了吸积盘的丰富的线光谱，而不限于仅两条先前已知的Si ii 6347和Si ii 6371线。估计圆盘光谱的预计旋转速度为180 km s-1。这样的值与吸积盘外层的开普勒旋转假设很好地吻合。修正后，发现在主食各阶段附近的所有吸收线的强度都有明显的增加，我们认为这是由于主食的光在其中一个喷流和/或增益器吸积盘上方的散射包络中被额外吸收的缘故。H α的V峰的净强度没有轨道变化，但可能具有271 d的周期性。R峰的净强度显示出轻微的轨道变化，并且在大约2780天的周期内缓慢变化。这些结果似乎支持了早期的结论，即H α发射起源于喷流状结构。结论.所有新的发现都支持当前的观点，即天琴座β的星周结构由厚的吸积盘、双极喷流和吸积盘上方的散射包层组成。
Context. Understanding large-scale mass exchange in binaries also requires studies of complicated objects in the rapid phases of the process. β Lyr is one such object. Aims. Our goals were to analyse 52 photographic and 651 electronic spectra of β Lyr to obtain additional information about circumstellar matter and to investigate spectrophotometric information for the first time. Methods. Improved quadratic ephemeris was derived via orbital solution with the FOTEL program. The spectra were disentangled using the KOREL program. Spectrophotometric quantities of 15 stronger absorption lines of the primary were measured and corrected for the orbital continuum variations using the fluxes calculated from a fit of the light curves with the BINSYN program. Central intensities of the V and R peaks of the Hα emission line were measured and corrected for the orbital light changes using the R-band light curve numerically modelled with the program PERIOD04. Results. Disentangling of photographic and electronic spectra led to the detection of weak absorption lines originating from the pseudophotosphere of the accretion disc. This way, a rich line spectrum of the accretion disc, not limited to only two previously known Si ii 6347 and Si ii 6371 lines, was obtained. A projected rotational velocity of 180 km s −1 was estimated for the disc spectrum. Such a value agrees well with the assumption of the Keplerian rotation of the outer layers of the accretion disc. After the correction, a pronounced increase of the strength of all absorption lines around phases of the primary eclipse was found. We argue that this is due to additional absorption of the light of the primary in one of the jets and/or scattering envelope above the accretion disc of the gainer. The net intensity of the V peak of Hα shows no orbital variation, but a possible 271-d periodicity. The net intensity of the R peak shows mild orbital changes and a slow change over a cycle of about 2780 days. These results seem to support the earlier conclusion that the Hα emission originates in the jet-like structures. Conclusions. All new findings support the current picture that the circumstellar structures of β Lyr consist of a thick accretion disc, bipolar jets, and a scattering envelope above the disc.