X级质子耀斑的特征研究

张烨; 师立勤; 崔延美; 刘四清

doi:10.11728/cjss2017.03.249

X级质子耀斑的特征研究

doi: 10.11728/cjss2017.03.249 cstr: 32142.14.cjss2017.03.249

1. 中国科学院国家空间科学中心北京 100190;
2. 中国科学院研究生院北京 100049

基金项目:

国家自然科学基金项目（11503063）和国家重点基础研究计划项目（2012CB825606）共同资助

详细信息

中图分类号: P353
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出版历程
- 收稿日期: 2016-03-02
- 修回日期: 2016-12-15
- 刊出日期: 2017-05-15

Research on Characteristics of X-class Solar Proton Flare

1. National Space Science Center, Chinese Academy of Sciences, Beijing 100190;
2. University of Chinese Academy of Sciences, Beijing 100049

摘要

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0.3J·m^-2，CME速度大于1300km·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.
- 质子耀斑 /
- 非质子耀斑 /
- 日冕物质抛射
Abstract: 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 X-ray 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 0.3J·m^-2 and CME speed is less than 1300km·s^-1. While proton flares are mostly located at central and western part, where X-ray integrated flux is greater than 0.3J·m^-2 and CME speed is greater than 1300km·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.
- Proton flare /
- Non-proton flare /
- Coronal Mass Ejection (CME)

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