织女星脉动的第一个证据？今天最广泛的光谱搜索结果
First evidence of pulsations in Vega? Results of today's most extensive spectroscopic search
摘要：
快速自转对恒星演化理论的影响至今仍知之甚少。织女星在这方面是一个特殊的对象，因为光谱和干涉测量研究表明，它是一个快速旋转器，接近极一，这是一种罕见的方向，特别是对地震研究感兴趣。在本文中，我们提出了第一个系统的搜索织女星脉动。目前的工作的目标是检测第一次在一个快速旋转的恒星看到近极的脉动。织女星监测准连续高分辨率阶梯光谱。在2008年、2009年和2010年的3次单独运行中，以高分辨率获得了总共4478个光谱。该数据集应代表迄今为止在Vega上获得的最广泛的高S/N、高分辨率准连续调查。计算了恒星光谱的等效光球吸收剖面，也计算了作为径向速度参考的大地线。对剩余速度进行了分析，并检测到可能表明恒星脉动的周期性低振幅变化。所有三个数据集均显示存在剩余周期变化：2008年为5.32和9.19 c/d（A约6 m/s），2009年为12.71和13.25 c/d（A约8 m/s），2010年为5.42和10.82 c/d（A约3-4 m/s）。对于2010年运行，对等效曲线的每个速度箱进行了Lomb-Scargle周期图，未显示存在任何高阶nrp模式。现在下结论说这些变化是由于恒星脉动造成的还为时过早，下一步必须用高度稳定的摄谱仪来确认探测结果。如果脉动被证实，它们非常小的振幅表明这颗恒星将属于一类非常“安静”的脉动。
英文摘要：
The impact of rapid rotation on stellar evolution theory remains poorly understood as of today. Vega is a special object in this context as spectroscopic and interferometric studies have shown that it is a rapid rotator seen nearly pole one, a rare orientation particularly interesting for seismic studies. In this paper we present a first systematic search for pulsations in Vega. The goal of the present work is to detect for the first time pulsations in a rapidly rotating star seen nearly pole-on. Vega was monitored in quasi-continuous high-resolution echelle spectroscopy. A total of 4478 spectra were obtained within 3 individual runs in 2008, 2009 and 2010 at high resolution. This data set should represent the most extensive high S/N, high resolution quasi-continuous survey obtained on Vega as of today. Equivalent photospheric absorption profiles were calculated for the stellar spectrum, but also for the telluric lines acting as a radial velocity reference. Residual velocities were analysed and periodic low amplitude variations, potentially indicative of stellar pulsations, detected. All three data sets revealed the presence of residual periodic variations: 5.32 and 9.19 c/d, (A approx 6 m/s) in 2008, 12.71 and 13.25 c/d, (A approx 8 m/s) in 2009 and 5.42 and 10.82 c/d, (A approx 3-4 m/s) in 2010. A Lomb-Scargle periodogram of each velocity bin of the equivalent profile was performed for the 2010 run, not showing the presence of any higher order nrp mode. It is too early to conclude that the variations are due to stellar pulsations, and a confirmation of the detection with a highly stable spectrograph is a necessary next step. If pulsations are confirmed, their very small amplitudes show that the star would belong to a category of very "quiet" pulsators.
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