论文标题
基于整个开普勒数据的主序列星级超级赛车
Main-sequence star super-flares based on entire Kepler data
论文作者
论文摘要
我们编写并使用了自动化的耀斑检测python脚本来搜索A，F，G，G，K和M型主序列中的超级风格，其中Kepler的长期数据从Q0到Q17。我们研究了超级赛车发生率的统计特性。对于G型数据集，我们将结果与Okamoto等人的先前结果进行了比较。 2021将数据集分为四个旋转频段。我们发现了针对耀斑频率分布的类似功率定律指数。因此，我们表明，包括高通滤波器，样品偏见，旋律学和耀斑检测的完整性没有意义，因为我们的结果与Okamoto等人相似。 2021年。我们估计，$ 10^{35} $ erg的G型矮人的超级漏斗每4360年一次出现在一颗星星上。我们在1896年的G型矮人中发现了4637个超级赛车。此外，我们在136、522、770和312型A型，F，K和M分别发现了321、1125、4538和5445 Super-Flares。我们发现，超级弹药与火炬能量的发生率（$ dn/de $），$ e $，显示具有$ dn/de \ propto e^{ - α} $的幂律分配，其中$α\ simeq $ 2.0至2.1 for f pypepe从F-Type到M型星星的光谱类型。相比之下，A型恒星获得的$α\ simeq $ 1.3表明，耀斑条件与其余光谱型恒星不同。我们注意到，F型在M型星中的耀斑发生率增加，而A型对F型恒星的降低。
We wrote and used an automated flare detection Python script to search for super-flares on main-sequence stars of types A, F, G, K, and M in Kepler's long-cadence data from Q0 to Q17. We studied the statistical properties of the occurrence rate of super-flares. For the G-type data set, we compared our results with the previous results of Okamoto et al. 2021 by splitting the data set into four rotational bands. We found similar power law indices for the flare frequency distribution. Hence, we show that inclusion of high-pass filter, sample biases, gyrochronology and completeness of flare detection is of no significance, as our results are similar to Okamoto et al. 2021. We estimated that a super-flare on G-type dwarfs of energy of $10^{35}$ erg occurs on a star once every 4360 years. We found 4637 super-flares on 1896 G-type dwarfs. Moreover, we found 321, 1125, 4538 and 5445 super-flares on 136, 522, 770 and 312 dwarfs of types A, F, K and M, respectively. We found that the occurrence rate ($dN/dE$) of super-flares versus flare energy, $E$, shows a power-law distribution with $dN/dE \propto E^{-α}$, where $α\simeq$ 2.0 to 2.1 for the spectral types from F-type to M-type stars. In contrast, the obtained $α\simeq$ 1.3 for A-type stars suggests that the flare conditions differ from the rest spectral-type stars. We note an increase in flare incidence rate in F-type to M-type stars and a decrease in A-type to F-type stars.
