论文标题
太阳能和恒星耀斑的概率分布功能
Probability Distribution Functions of Solar and Stellar Flares
论文作者
论文摘要
我们研究了太阳耀斑的软X射线数据，发现耀斑通力的分布功能是通过锥形功率定律或伽马功能分布成功建模的，其功率指数略小于2，这表明耀斑群的总能量主要是由少量大型耀斑造成的。预计在1000年内，最大的太阳能耀斑在X70左右的速度较大。我们还从太阳能型星中研究了超级流（比太阳能耀斑更具势力），并发现它们在伽马功能分布拟合中的功率指数约为1.05，比太阳能耀斑的扁平弹力要稍微得多。向下推断的恒星耀斑能量的分布函数与太阳能耀斑能的分布函数连接。
We studied the soft X-ray data of solar flares and found that the distribution functions of flare fluence are successfully modeled by tapered power law or gamma function distributions whose power exponent is slightly smaller than 2, indicating that the total energy of the flare populations is mostly contributed from a small number of large flares. The largest possible solar flares in 1000 years are predicted to be around X70 in terms of the GOES flare class. We also studied superflares (more energetic than solar flares) from solar-type stars, and found that their power exponent in the fitting of the gamma function distribution is around 1.05, much flatter than solar flares. The distribution function of stellar flare energy extrapolated downward does not connect to the distribution function of solar flare energy.
