X级质子耀斑的特征研究

发布时间：2018-04-30 15:15

本文选题：质子耀斑 + 非质子耀斑　；参考：《空间科学学报》2017年03期

【摘要】：为了更加准确地判断X级耀斑是否引发质子事件,对X级质子耀斑和非质子耀斑的耀斑积分通量、源区、CME速度、CME角宽度、背景太阳风速度及背景X射线通量的分布进行了统计研究.发现非质子耀斑和质子耀斑的积分通量、经度、CME速度和CME角宽度具有明显不同的分布.非质子耀斑大多集中在东部,耀斑积分通量小于0.3J·m~(-2),CME速度小于1300km·s~(-1)的区域内;质子耀斑大多集中在中部或西部,耀斑积分通量大于0.3 J·m~(-2),CME速度大于1300 km·s~(-1)的区域内.质子耀斑伴随的CME角宽度主要集中在360°,非质子耀斑的CME角宽度分布则相对分散.两类耀斑的背景太阳风速度和背景X射线通量分布差别不大.利用两类耀斑各个参量分布上的差异,有望提高X级耀斑预报的准确率.
[Abstract]:In order to determine more accurately whether X class flares cause proton events, the integral flux of X class proton flares and non-proton flares, the source region CME velocity and the width of CME angle are calculated. The distribution of background solar wind velocity and background X ray flux is studied statistically. It is found that the integral flux, longitude velocity and CME angular width of non-proton flare and proton flare have different distributions. Most of the non-proton flares are concentrated in the east, the integral flux of the flares is less than 0.3 J / m ~ (-1) and the velocity of the proton flare is more than 1300 km / s ~ (-1) in the central or western part of the region, and the integral flux of the flare is more than 1300 km / s ~ (-1). The CME angular width of proton flares is mainly concentrated at 360 掳, while the CME angular width distribution of non-proton flares is relatively dispersed. The velocity of background solar wind and the distribution of background X ray flux of the two flares are not different. It is expected to improve the accuracy of X class flares prediction by using the differences in the distribution of each parameter between the two flares.
【作者单位】：中国科学院国家空间科学中心;中国科学院研究生院;
【基金】：国家自然科学基金项目(11503063) 国家重点基础研究计划项目(2012CB825606)共同资助
【分类号】：P353

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