本文選題：質子耀斑 + 非質子耀斑��； 參考：《空間科學學報》2017年03期

【摘要】：為了更加準確地判斷X級耀斑是否引發(fā)質子事件,對X級質子耀斑和非質子耀斑的耀斑積分通量、源區(qū)、CME速度、CME角寬度、背景太陽風速度及背景X射線通量的分布進行了統(tǒng)計研究.發(fā)現(xiàn)非質子耀斑和質子耀斑的積分通量、經(jīng)度、CME速度和CME角寬度具有明顯不同的分布.非質子耀斑大多集中在東部,耀斑積分通量小于0.3J·m~(-2),CME速度小于1300km·s~(-1)的區(qū)域內;質子耀斑大多集中在中部或西部,耀斑積分通量大于0.3 J·m~(-2),CME速度大于1300 km·s~(-1)的區(qū)域內.質子耀斑伴隨的CME角寬度主要集中在360°,非質子耀斑的CME角寬度分布則相對分散.兩類耀斑的背景太陽風速度和背景X射線通量分布差別不大.利用兩類耀斑各個參量分布上的差異,有望提高X級耀斑預報的準確率.
[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 擄, 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.
【作者單位】： 中國科學院國家空間科學中心;中國科學院研究生院;
【基金】：國家自然科學基金項目(11503063) 國家重點基礎研究計劃項目(2012CB825606)共同資助
【分類號】：P353

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1 王家龍;太陽質子耀斑的一個統(tǒng)計性質[J];空間科學學報;1993年04期

2 林華安,王世金;太陽質子耀斑X射線輻射特征及質子事件警報[J];空間科學學報;1993年02期

3 ;[J];;年期

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本文編號：1825068