X级质子耀斑的特征研究

Research on Characteristics of X-class Solar Proton Flare

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.

Solar Proton Events（SPE） often accompany with solar flares,and the probability that solar proton events triggered by X-class flares is larger than that triggered by other types of flares.In order to improve the forecast accuracy of solar proton events triggered by X-class flares,the relation between proton/non-proton flares and space environmental parameters,including X-ray integrated flux,source region,CME speed,CME angle width,ambient solar wind speed,and ambient Xray flux,are analyzed statistically.The results show that the distributions of X-ray integrated flux,heliolongitude,CME speed,and CME angle width are different for non-proton and proton flares.Non-proton flares are mostly located at eastern part,where X-ray integrated flux is less than 0.3 J·m^（-2） and CME speed is less than 1300 km·s^（-1）.While proton flares are mostly located at central and western part,where X-ray integrated flux is greater than 0.3 J·m^（-2） and CME speed is greater than 1300 km·s^（-1）.Furthermore,halo CMEs are often associated with proton flares,while angle width distribution of CMEs that accompanied with non-proton flares is relatively disperse.For proton and non-proton flares,the distribution of their ambient solar wind speed and ambient X-ray flux are similar.According to the different characteristics of the SPEs for proton and non-proton flares,the accuracy of SPE forecast can be improved.