论文标题
GD 99：旧ZZ CETI伴侣的重新调查
GD 99: Re-investigation of an old ZZ Ceti companion
论文作者
论文摘要
语境。由于光度法任务，我们可以访问有关白矮星恒星（尤其是脉动恒星）特性的越来越多的信息。就脉动器而言，我们有机会通过星空学的手段深入了解其原本隐藏的内饰。除了基于空间的观察外，我们还利用了从地面研究白矮星恒星的脉动的机会，要么是对基于空间的测量值进行互补的观测值，要么是在长时间尺度上对所选目标的单个观察跑步。 目标。我们旨在研究明亮但几乎没有研究的ZZ CETI Star（GD 99）的长期单位观察。我们的主要目标是确定尽可能多的Atterosemodicologology的本征模，然后对该目标进行地震分析。 方法。我们对在不同时期中获得的光曲线进行了傅立叶分析。在找到了脉动的正常模式后，我们运行了2018年版的白矮人演变代码，以为周期拟合构建模型网格。我们将最佳拟合模型的地震距离与Gaia测量提供的几何值进行了比较。 结果。我们发现GD 99在200-1100 s的周期范围内具有丰富的脉动模式，因为我们发现了七个新时期。与文献数据一起，我们能够使用11个模式进行纯种曲线。我们接受了TEFF = 13 500 K，M* = 0.80 MSUN作为最佳拟合度的Ateroseasic模型解决方案，但是，这表明比基于光谱值所预期的更热，更庞大的恒星。我们还根据苔丝观测值估计，恒星的旋转速率为13.17 h。
Context. Thanks to photometric space missions, we have access to more and more information on the properties of white dwarf stars, especially pulsating ones. In the case of pulsators, we have the opportunity to get an insight into their otherwise hidden interiors by the means of asteroseismology. In addition to space-based observations, we also take advantage of the opportunity to study the pulsations of white dwarf stars from the ground, either as observations that are complementary to space-based measurements or individual observing runs on selected targets across long timescales. Aims. We aim to investigate long-term, single-site observations of the bright, yet scarcely studied ZZ Ceti star, GD 99. Our main goals are to determine as many eigenmodes for asteroseismology as possible and then to carry out a seismic analysis of this target. Methods. We performed a Fourier analysis of the light curves obtained in different epochs. After finding the normal modes of the pulsation, we ran the 2018 version of the White Dwarf Evolution Code to build model grids for the period fits. We compared the seismic distance of the best-fit model with the geometric value provided by Gaia measurements. Results. We find that GD 99 is rich in pulsation modes in the 200-1100 s period range, as we detected seven new periods. Together with the literature data, we were able to use 11 modes for the asteroseismic fits. We accepted an asteroseismic model solution with Teff = 13 500 K and M* = 0.80 Msun as a best fit, however, this suggests a hotter and more massive star than we might have expected based on the spectroscopic values. We also estimated the rotational rate of the star to be 13.17 h, based on TESS observations.
