根据层析分析推断的V926 Sco吸积盘的可变性
Variability of the accretion disk of V926 Sco inferred from tomographic analysis
摘要：
我们目前的相位分辨光谱观测的低质量X射线双星V926斯科（4U 1735-44），覆盖轨道周期为0.23天，获得与沃尔特巴德6.5米麦哲伦望远镜在拉斯坎帕纳斯天文台在2010年6月和2011年6月。我们使用H $α$径向速度推导出系统速度为-109 $\pm$ 4 km s $^{-1}$。在我们的观测过程中，与以前的作者共同观察到的谱线的半高宽明显较低，表明系统中的速度大大降低。在我们的观测过程中，相对于He II $λ$ 4686的Bowen荧光线的等效宽度比以前报道的系统低两个或更多，这表明次级辐射减少。H $α$和He II $λ$ 4686的多普勒和调制断层扫描显示了不对称的发射，这可以归因于吸积盘的凸起，这是从以前的作者的He II观测中推断出来的。在我们的观测中，与2003年进行的光学观测相比，在与光学观测同时进行的时间内，来自源的X射线通量显着降低。我们认为，该系统是在一个较低的吸积状态相比，早期的观察，这既解释了从磁盘上观察到的较低的速度和减少由于鲍文荧光检测到的排放从二次。
英文摘要：
We present phase-resolved spectroscopic observations of the low-mass X-ray binary V926 Sco (4U 1735-44), covering the orbital period of 0.23d, obtained with the Walter Baade 6.5m Magellan Telescope at the Las Campanas Observatory in June 2010 and June 2011. We use H$α$ radial velocities to derive a systemic velocity of -109 $\pm$ 4 km s$^{-1}$. The FWHM of the lines observed in common with previous authors are significantly lower during our observations suggesting much reduced velocities in the system. The equivalent width of the Bowen fluorescence lines with respect to He II $λ$4686 are factors of two or more lower during our observations in comparison to those previously reported for the system, suggesting reduced irradiation of the secondary. Doppler and modulation tomography of H$α$ and He II $λ$4686 show assymmetric emission that can be attributed to a bulge in the accretion disk, as inferred from He II observations by previous authors. The X-ray fluxes from the source at times concurrent with the optical observations are significantly lower during our observations than during optical observations taken in 2003. We suggest that the system is in a lower accretion state compared to earlier observations; this explains both the lower velocities observed from the disk and the reduction of emission due to Bowen fluorescence detected from the secondary.
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