论文标题
南半球的$ \ it tess $的太阳能星星的超级流量和可变性
Superflares and Variability in Solar-Type Stars with $\it TESS$ in the Southern Hemisphere
论文作者
论文摘要
自从$ \ it Kepler $推出以来，太阳能型星的超级流域一直是一个迅速发展的领域。多年来，已经进行了几项研究，研究了这些爆炸性事件的统计数据。在这项研究中，我们介绍了使用2分钟的节奏在整个南半球的$ \ it tess $中使用光度数据制成的太阳能型星的恒星耀斑的统计分析（部门1-13）。由于表面上的大星点，我们从光弯曲中存在的旋转调制中得出了样品中所有恒星的旋转周期。我们从209个太阳能型恒星中识别出1980年的恒星耀斑，其能量范围在$ 10^{31} -10^{36} $ erg（使用太阳耀斑分类，这对应于X1- x100,000），并对其性质进行分析。我们研究了耀斑的旋转相，并且没有发现任何阶段的偏好，表明耀斑是随机分布的。作为基准，我们使用太阳耀斑的数据来详细介绍太阳耀斑和黑子之间的密切关系。此外，我们还计算每个恒星的近似斑点区域，并将其与耀斑数，旋转相和耀斑能量进行比较。此外，在连续的观察区中观察到了我们的两个恒星，其光曲面跨越了一年，因此，我们更详细地检查了这些恒星的出色变异性。
Superflares on solar-type stars has been a rapidly developing field ever since the launch of $\it Kepler$. Over the years, there have been several studies investigating the statistics of these explosive events. In this study, we present a statistical analysis of stellar flares on solar-type stars made using photometric data in 2-min cadence from $\it TESS$ of the whole southern hemisphere (sectors 1 - 13). We derive rotational periods for all stars in our sample from rotational modulations present in the lightcurve as a result of large starspot(s) on the surface. We identify 1980 stellar flares from 209 solar-type stars with energies in the range of $10^{31} - 10^{36}$erg (using the solar flare classification, this corresponds to X1 - X100,000) and conduct an analysis into their properties. We investigate the rotational phase of the flares and find no preference for any phase suggesting the flares are randomly distributed. As a benchmark, we use GOES data of solar flares to detail the close relationship between solar flares and sunspots. In addition, we also calculate approximate spot areas for each of our stars and compare this to flare number, rotational phase, and flare energy. Additionally, two of our stars were observed in the continuous viewing zone with lightcurves spanning one year, as a result, we examine the stellar variability of these stars in more detail.
