Asteroseismology based on high time-resolution and high dispersion spectroscopy

在roAp恒星中发现的振荡的垂直波长非常短，以至于每条光谱线变化的幅度和相位高度依赖于谱线轮廓的水平。在考虑成线层厚度有限的情况下，进行了线形变化的数值模拟。我们证明了这种治疗是多么有效。对开普勒观测时间的质心修正打破了数据的常规时间采样。其结果是，奈奎斯特别名被分成了多组，可以通过形状来识别。我们对这一现象进行了分析推导，同时用模拟的和真实的开普勒数据进行了演示。观测表明，当恒星旋转速度低于分裂速度时，恒星周围会形成一个星周盘。我提出了一个可行的假设，通过考虑漏波对角动量转移的影响来解释这个谜团。

The vertical wavelengths of the oscillations found in roAp stars are so short that the amplitude and phase of the variation of each spectroscopic line are highly dependent on the level of the line profile. We carried out a numerical simulation of line-profile variation by taking account of the finite thickness of the line-forming layer. We demonstrated how effective this treatment is.Barycentric corrections made to the timing of Kepler observations break the regular time-sampling of the data. A consequence is that Nyquist aliases are split into multiplets that can be identified by their shape. We provided an analytical derivation of the phenomenon, alongside demonstrations with simulated and real Kepler data.Observations indicate that a circumstellar disk is formed around a Be star while the stellar rotation is below the break-up velocity. I proposed a working hypothesis to explain this mystery by taking account of the effect of leaky waves upon angular momentum transfer.