太阳X级耀斑及相关现象研究

发布时间：2018-02-13 18:14

本文关键词： 太阳活动周太阳耀斑太阳质子事件超级活动区　出处：《南京信息工程大学》2013年硕士论文　论文类型：学位论文

【摘要】：依据X级以上耀斑的数据,我们统计分析了21-23周期间不同强度X级以上耀斑的统计分布、太阳周分布特征以及与超级活动区的关系。分析结果表明： 1.X1.0-X1.9、X2.0-X2.9、X3.0-X4.9、X5-X9.9和X10级以上耀斑分别占X级以上耀斑总数的52.71%、20.59%、13.57%、8.37%和4.75%。22周X级以上耀斑集中分布在太阳活动周峰值附近,而23周X级以上耀斑的分布比较分散。21周X级以上耀斑的分布既不像22周那么集中,也不像23周那么分散。在21-23周期间,32.2%的X1.0-X1.9、31.9%的X2.0-X2.9耀斑、43.3%的X3.0-X4.9耀斑、81.08%的X5.0-X9.9耀斑和95.2%的X10以上耀斑是由超级活动区产生的。 2.21-23周共有58个X5级以上的耀斑,上升段总共只有5个,占总数的8.6%,91.4%的X5级以上耀斑出现在太阳活动周的下降段。从数量上看,21与22周X5级以上耀斑无南北不对称性,第23周有非常明显的南北不对称性,X5以上耀斑主要集中在南半球。21周X5以上的耀斑有明显的东西不对称性,耀斑主要集中出现在东半球,22与23周无东西不对称性。从时间和纬度上看,则每一个太阳活动周的不同阶段,X5以上的耀斑都存在不对称性。X5以上的耀斑主要集中在4个经度带,分别为70～110°,131～199°,200～260°和281～360°,这四个经度带分别产生了10个,11个,15和18个X5级以上的耀斑。 3.X1级耀斑相对太阳黑子数在21和22周均提前了一个月,而在第23周则延迟了13个月；X2级以上耀斑与太阳黑子数在21延迟了9个月,在22周提前了一个月,而在第23周则延迟了32个月。依据太阳质子事件的数据,我们统计分析了21-23周的太阳质子事件,统计分析结果如下： 1.无论是2级还是3级太阳质子事件,多数都出现在太阳活动周的下降段。太阳质子事件越强,太阳活动周越弱,出现在太阳活动周下降段的比率越高。在22周,2级、3级和3级以上太阳质子事件聚集在太阳活动周峰值附近的现象非常突出。22周太阳活动峰值及之后的时段,2级、3级和3级以上太阳质子事件中的相当一部分的源区在北半球30°以上的区域。 2.GLE事件增长率超过100%事件的源区位置大约为W25°到W90°,其中60°左右的位置具有最大的增长率,而最强的非相对论太阳质子事件源区位置为E30°到W20°。 3.2级、3级和3级以上太阳质子事件在太阳活动周期间可能出现1-3个峰值。无论对于2级太阳质子事件,还是3级和3级以上太阳质子事件在第23周都出现了3个峰值,且大的峰值都出现在太阳黑子数描述的太阳活动峰值之后,即2级、3级和3级以上太阳质子事件频次最高的时期出现在太阳活动周的下降段,而且有一个峰值出现在太阳活动峰值的之后的第5年。
[Abstract]:Based on the data of flares above grade X, the statistical distribution of flares with different intensities over class X during 21-23 weeks, the characteristics of solar circumference and the relationship between the distribution of solar flares and the superactive regions are analyzed statistically. The results show that:. 1.X1.0-X1.9X 2.0-X2.9N X3.0-X4.9N X5-X9.9 and over X10 flares account for 52.71% of the total number of flares above class X, respectively. The flares of grade X and above are distributed in the vicinity of the peak values of the solar cycle, respectively, at 20.59 and 13.577.37% and 4.75.22 weeks, respectively. The distribution of flares above class X at 23 weeks was scattered. The distribution of flares above class X at week 21 was not as concentrated as that in week 22. During the 21-23 weeks, 32.2% X1.0-X1.91.9% X2.0-X2.9 flares 43.3% X3.0-X4.9 flares 81.08% X5.0-X9.9 flares and 95.2% flares above X10 are produced by superactive regions. 2.21-23 weeks there were 58 flares of grade X 5 or above, and only 5 of the rising flare, accounting for 91.4% of the total, appeared in the descending segment of the solar cycle. There was no north-south asymmetry in the number of flares above grade X5 for weeks 21 and 22. In the 23rd week, there was a very obvious north-south asymmetry of the flare over X5, mainly concentrated in the Southern Hemisphere .21 weeks. The flares above X5 had obvious east-west asymmetry. The flares are mainly concentrated in the Eastern Hemisphere 22 and 23 cycles without east-west asymmetry. From the point of view of time and latitude, the flare above X 5 at different stages of each solar cycle has asymmetry. The flares above X 5 are mainly concentrated in 4 longitude bands. These four longitude zones have 10 flares, 11 zon15 flares and 18 X 5 flares, respectively. 3. The number of solar spots of class X1 is one month earlier than the number of sunspots in weeks 21 and 22, while the flare and sunspot number of class X2 and sunspot are delayed by 13 months in week 23 and by nine months in 21 and one month in week 22. In week 23, the delay was 32 months. Based on the data of solar proton events, we statistically analyze the solar proton events of 21-23 weeks. The results are as follows:. 1. Most of the solar proton events, whether of order 2 or 3, occur in the descending segment of the solar cycle. The stronger the solar proton event, the weaker the solar cycle. The higher the rate of the fall in the solar cycle, the higher the concentration of solar proton events near the peak of the solar cycle around the peak of the solar cycle in cycle 22 and beyond. A considerable portion of the solar proton events of order 3 and above are located above 30 掳in the Northern Hemisphere. 2. The growth rate of GLE events is higher than that of 100% events. The source region of GLE events is about W25 掳to W90 掳, in which about 60 掳has the largest growth rate, while the strongest source of non-relativistic solar proton events is E30 掳to W20 掳. The solar proton events of order 3.2 and above may have 1-3 peaks during the solar active cycle. Whether for the second order solar proton events or the third or higher solar proton events, there are 3 peaks in the 23rd week. And the large peaks occur after the peak of solar activity described by sunspot number, that is, the period of the highest frequency of solar proton events of order 2 and above appears in the descending section of the solar cycle. And there is a peak in the fifth year after the peak of solar activity.
【学位授予单位】：南京信息工程大学
【学位级别】：硕士
【学位授予年份】：2013
【分类号】：P182.52

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