本文關鍵詞： 太陽活動周 太陽耀斑 太陽質子事件 超級活動區(qū)　出處：《南京信息工程大學》2013年碩士論文　論文類型：學位論文

【摘要】：依據(jù)X級以上耀斑的數(shù)據(jù),我們統(tǒng)計分析了21-23周期間不同強度X級以上耀斑的統(tǒng)計分布、太陽周分布特征以及與超級活動區(qū)的關系。分析結果表明： 1.X1.0-X1.9、X2.0-X2.9、X3.0-X4.9、X5-X9.9和X10級以上耀斑分別占X級以上耀斑總數(shù)的52.71%、20.59%、13.57%、8.37%和4.75%。22周X級以上耀斑集中分布在太陽活動周峰值附近,而23周X級以上耀斑的分布比較分散。21周X級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周期間,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以上耀斑是由超級活動區(qū)產生的。 2.21-23周共有58個X5級以上的耀斑,上升段總共只有5個,占總數(shù)的8.6%,91.4%的X5級以上耀斑出現(xiàn)在太陽活動周的下降段。從數(shù)量上看,21與22周X5級以上耀斑無南北不對稱性,第23周有非常明顯的南北不對稱性,X5以上耀斑主要集中在南半球。21周X5以上的耀斑有明顯的東西不對稱性,耀斑主要集中出現(xiàn)在東半球,22與23周無東西不對稱性。從時間和緯度上看,則每一個太陽活動周的不同階段,X5以上的耀斑都存在不對稱性。X5以上的耀斑主要集中在4個經度帶,分別為70～110°,131～199°,200～260°和281～360°,這四個經度帶分別產生了10個,11個,15和18個X5級以上的耀斑。 3.X1級耀斑相對太陽黑子數(shù)在21和22周均提前了一個月,而在第23周則延遲了13個月；X2級以上耀斑與太陽黑子數(shù)在21延遲了9個月,在22周提前了一個月,而在第23周則延遲了32個月。 依據(jù)太陽質子事件的數(shù)據(jù),我們統(tǒng)計分析了21-23周的太陽質子事件,統(tǒng)計分析結果如下： 1.無論是2級還是3級太陽質子事件,多數(shù)都出現(xiàn)在太陽活動周的下降段。太陽質子事件越強,太陽活動周越弱,出現(xiàn)在太陽活動周下降段的比率越高。在22周,2級、3級和3級以上太陽質子事件聚集在太陽活動周峰值附近的現(xiàn)象非常突出。22周太陽活動峰值及之后的時段,2級、3級和3級以上太陽質子事件中的相當一部分的源區(qū)在北半球30°以上的區(qū)域。 2.GLE事件增長率超過100%事件的源區(qū)位置大約為W25°到W90°,其中60°左右的位置具有最大的增長率,而最強的非相對論太陽質子事件源區(qū)位置為E30°到W20°。 3.2級、3級和3級以上太陽質子事件在太陽活動周期間可能出現(xiàn)1-3個峰值。無論對于2級太陽質子事件,還是3級和3級以上太陽質子事件在第23周都出現(xiàn)了3個峰值,且大的峰值都出現(xiàn)在太陽黑子數(shù)描述的太陽活動峰值之后,即2級、3級和3級以上太陽質子事件頻次最高的時期出現(xiàn)在太陽活動周的下降段,而且有一個峰值出現(xiàn)在太陽活動峰值的之后的第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 擄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 擄to W90 擄, in which about 60 擄has the largest growth rate, while the strongest source of non-relativistic solar proton events is E30 擄to W20 擄. 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.
【學位授予單位】：南京信息工程大學
【學位級別】：碩士
【學位授予年份】：2013
【分類號】：P182.52

【參考文獻】

相關期刊論文 前1條

1 李可軍,洪琴芳,顧嘯馬;日面高緯黑子與太陽活動[J];天文學報;1999年04期

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本文編號：1508789