中间极性分子DQ Her的自旋分辨光谱
Spin-resolved spectroscopy of the intermediate polar DQ Her
摘要：
我们提出了高速光谱观测的中间极性DQ武仙座。两条He I线的多普勒层析成像揭示了白矮星主星周围吸积盘中的螺旋密度结构。这些螺旋看起来非常类似于矮新星爆发时所看到的螺旋。DQ Her是第一个建立良好的中间极性，其中可以看到螺旋，由于系统的高质量传递速率，螺旋还可能持续存在。螺旋结构给出了另一种解释的WD自旋频率的边带中发现IP光变曲线。He II 4686的多普勒断层图像显示，大部分发射不是盘状的。自旋拖尾的光谱揭示了一个脉动的He II 4686的排放，被认为是由于再处理的X射线从白矮星的磁极在吸积流接近WD。我们证实了以前的发现，脉动是唯一可见的红移部分的线时，光束点的背面的光盘。光盘正面没有经过再处理的光可以用光盘前边缘的遮蔽来解释，但是光盘背面蓝移的光没有额外的发射是令人困惑的。在吸积幕中的再处理可能是这个问题的答案，也可以解释在He II 4686线中发现的高度非开普勒速度分量。我们的自旋轨迹可以对未来的吸积幕模型形成强有力的测试，有可能区分71秒或142秒的自旋周期。在选定的轨道相位上拍摄的自旋轨迹数据显示，几乎没有证据表明亮点对脉动有重大贡献，这使我们能够排除最近提出的71秒是拍频周期和70.8秒是自旋周期的建议。
英文摘要：
We present high-speed spectroscopic observations of the intermediate polar DQ Herculis. Doppler tomography of two He I lines reveals a spiral density structure in the accretion disc around the white dwarf primary. The spirals look very similar to the spirals seen in dwarf novae during outburst. DQ Her is the first well established intermediate polar in which spirals are seen, that are in addition likely persistent because of the system's high mass transfer rate. Spiral structures give an alternative explanation for sidebands of the WD spin frequency that are found in IP light curves. The Doppler tomogram of He II 4686 indicates that a large part of the emission is not disc-like. Spin trails of spectra reveal a pulsation in the He II 4686 emission that is believed to result from reprocessing of X-rays from the white dwarf's magnetic poles in the accretion flow close to the WD. We confirm the previous finding that the pulsation is only visible in the red-shifted part of the line when the beam points to the back side of the disc. The absence of reprocessed light from the front side of the disc can be explained by obscuration by the front rim of the disc, but the absence of extra emission from the blue-shifted back side of the disc is puzzling. Reprocessing in accretion curtains can be an answer to the problem and can also explain the highly non-Keplerian velocity components that are found in the He II 4686 line. Our spin trails can form a strong test for future accretion curtain models, with the possibility of distinguishing between a spin period of 71s or 142s. Spin trails of data taken at selected orbital phases show little evidence for a significant contribution of the bright spot to the pulsations and allow us to exclude a recent suggestion that 71s is the beat period and 70.8s the spin period.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
