太阳活动峰年和谷年期间黑子群与耀斑的统计分析
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摘要
基于NOAA/SWPC公布的太阳活动数据,我们选取第24太阳活动峰年附近的12个连续月份(2011年7月至2012年6月)和第23太阳活动周谷年附近的12个连续月份(2005年7月至2006年6月),统计了这两段时间中太阳黑子群和耀斑的活动规律,并根据时间、黑子群分布纬度、寿命和磁场类型等对峰年和谷年进行了详细分析和比较,主要结论如下所述.(1)黑子群数随时间的变化在峰年和谷年均比较随机,峰年期间黑子数比谷年增多1.5倍左右.耀斑爆发与黑子群活动具有良好的相关性,但峰年期间存在某个月份耀斑数很少的现象,而谷年期间存在某个月份耀斑数集中增多的现象.(2)无论峰年还是谷年,δ类型黑子群的耀斑产率(耀斑总数与黑子群总数之比)最大,但β型黑子群产生的耀斑爆发最多.耀斑产率与磁场类型有密切关系,但与其所处太阳活动周中的阶段无关.(3)黑子群和耀斑的纬度分布的南北不对称性,以X级耀斑最为显著.峰年较谷年的耀斑数增加主要集中在C级和M级.(4)耀斑产率同黑子群寿命具有良好的相关性,但黑子群的数目同它们的寿命之间没有明显的规律.
Based on the NOAA/SWPC data, by choosing two separative periods with successive 12 months, that is, 2005 July–2006 June(during the solar minimum) and 2011 July–2012 June(during the solar maximum), we analyze the activity of flares and compare the statistical results between the two periods for studying their evolution with time, sunspot distribution, sunspot lifetime and magnetic field types. The main conclusions are:(1) The time variation of sunspot groups number is random for both the solar minimum and maximum periods. The sunspot number during the solar maximum is about 1.5 times larger than during the solar minimum. The flare number shows good correlation with the sunspot group number. During solar maximum there may be very few flares for some months, while during solar minimum there can be plenty of flares for some months, indicating the importance of keeping monitoring for solar activities even during the solar minimum period.(2) The δ-sunspot groups have the highest flare productivity(the ratio of flare amount to sunspot group number) for both solar minimum and maximum, while the β-sunspot groups have produced the most flares. The flare productivity of sunspot groups has close relation with magnetic field type, and it has no obvious relation with the state of solar cycle.(3) There is serious asymmetry in the distribution for flares, especially for X-class flares. The increase of the flares number from solar minimum to maximum is mainly caused by C- and M-class flares.(4) The number of sunspot groups has no obvious correlation with their lifetime, while the flare productivity shows well correlation with sunspot lifetime for all periods.
Based on the NOAA/SWPC data, by choosing two separative periods with successive 12 months, that is, 2005 July–2006 June(during the solar minimum) and 2011 July–2012 June(during the solar maximum), we analyze the activity of flares and compare the statistical results between the two periods for studying their evolution with time, sunspot distribution, sunspot lifetime and magnetic field types. The main conclusions are:(1) The time variation of sunspot groups number is random for both the solar minimum and maximum periods. The sunspot number during the solar maximum is about 1.5 times larger than during the solar minimum. The flare number shows good correlation with the sunspot group number. During solar maximum there may be very few flares for some months, while during solar minimum there can be plenty of flares for some months, indicating the importance of keeping monitoring for solar activities even during the solar minimum period.(2) The δ-sunspot groups have the highest flare productivity(the ratio of flare amount to sunspot group number) for both solar minimum and maximum, while the β-sunspot groups have produced the most flares. The flare productivity of sunspot groups has close relation with magnetic field type, and it has no obvious relation with the state of solar cycle.(3) There is serious asymmetry in the distribution for flares, especially for X-class flares. The increase of the flares number from solar minimum to maximum is mainly caused by C- and M-class flares.(4) The number of sunspot groups has no obvious correlation with their lifetime, while the flare productivity shows well correlation with sunspot lifetime for all periods.
引文
1 Hale G,Nicholson S.Magnetic Observations of Sunspots,1917-1924.Washington D C:Carnegie Institution of Washington,1938
2 McIntosh P S.The classification of sunspot groups.Solar Phys,1990,125:251–267
3 Wheatland M S.Rates of flaring in individual active regions.Solar Phys,2001,203:87–106
4 Giovanelli R G.The relations between eruptions and sunspots.Astrophys J,1939,89:555–567
5 Greatrix G R.On the statistical relations between flare intensity and sunspots.Mon Not Roy Astron Soc,1963,126:123–133
6 Kildahl K.In:Solar-Terrestrial Predictions Proceedings 3.Boulder Colorado:U S Dept Commerce,1980.166–166
7 Atac T.Statistical relationship between sunspots and major flares.Astrophys Space Sci,1987,129:203–208
8 Bornmann P L,Shaw D.Flare rates and the McIntosh active-region classifications.Solar Phys,1994,150:127–146
9 Sammis I,Tang F,Zirin H.The dependence of large flare occurrence on the magnetic structure of sunspots.Astrophys J,2000,540:583–587
10 Zhang H.Magnetic shear of a large delta sunspot group(NOAA 6659)in June 1991.Astron Astrophys,1995,297:869–880
11 Liu Y,Zhang H.Relationship between magnetic evolution and major flare event on July 14.Astron Astrophys,2001,372:1019–1029
12 Liu Y,Zhang H.Analysis of delta spot.Astron Astrophys,2002,386:646–652
13 Chumak O V,Chumak Z N.A stochastic method of describing the evolution of solar active regions(in Russian).Kinematika i Fizika Nebesnykh Tel,1987,3:7–13
14 Guo J,Zhang H Q,Chumak O V,et al.A quantitative study on magnetic configuration for active regions.Solar Phys,2006,237:25–43
15 Guo J,Zhang H Q,Chumak O V,et al.The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle.Mon Not R Astron Soc,2010,405:111–114
16 Cui Y M,Li R,Zhang L Y,et al.Correlation between solar flare productivity and photospheric magnetic field properties.Solar Phys,2006,237:45–59
17 Yang X,Zhang H Q,Gao Y,et al.A statistical study on photospheric magnetic nonpotentiality of active regions and its relationship with flares during solar cycles 22-23.Solar Phys,2012,280:165–181
18 Zirin H,Liggett M A.Delta spots and great flares.Solar Phys,1987,133:267–283
19 Jakimiec M,Paciorek J,Bartkowiak A.A multivariate comparison of delta and of other magnetic class sunspot groups.Acta Astron,1991,41:61–71
20 Shi Z,Wang J.Delta-sunspots and X-class flares.Solar Phys,1994,149:105–118
21 Achong A,Stahl P A.SID flare production is independent of Mt.Wilson magnetic class.Solar Phys,1984,92:259–269
22 Ternullo M,Contarino L,Romano P,et al.A statistical analysis of sunspot groups hosting M and X flares.Astron Nachr,2006,327:36–43
23 Kno ska S,Kr ivsky`L.Types of sunspots,magnetic classification and flare yield in cycle no.20.Bull Astron Inst Czech,1981,32:292–303
24 Chen A Q,Wang J X,Li J W,et al.Statistical properties of superactive regions during solar cycles 19-23.Astron Astrophys,2011,534:47–55
25 Gupta M,Mishra V K,Mishra A P.Solar activity parameters and their interrelationship:Continuous decrease in flare activity from solar cycles 20to 23.J Geophys Res,2007,112:A05105
26 Zharkov S I,Zharkova V V.Statistical properties of Hαflares in relation to sunspots and active regions in the cycle 23.J Atmosph Solar-Terrestrial Phys,2011,73:264–270
27 Zhang L Y,Cui Y M,He Y L,et al.Longitudinal distribution of major solar flares during 1975-2005.Adv Spa Res,2007,40:970–975
28 Leif Svalgaard L,Cliver E W,Kamide Y.Sunspot cycle 24:Smallest cycle in 100 years?Geophys Res Lett,2005,32(1):L01104
29 Bell B,Glazer H.Some sunspot and flare statistics.Smithsonian Contr Astrophys,1959,3:25–38
30 Feldman U,Doschek G A,Klimchuk J A.The occurrence rate of soft X-Ray flares as a function of solar activity.Astrophys J,1997,474:511–517
31 Yin S Y,Chen P F,Ding M D,et al.A statistical study of soft X-ray flares during solar cycle 22(in Chinese).J Nanjing Univ(Nat Sci),2002,38:458–461[尹素英,陈鹏飞,丁明德,等.第22太阳活动周软X射线耀斑的统计研究.南京大学学报(自然科学),2002,38:458–461]
32 Ternullo M,Zuccarello F,Contarino L,et al.A statistical approach to the spot-flare connection.In:the Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188.Netherlands:ESA Publications Division,2002.591–594
1)因为强度超过了探测器极限,根据外推得到的等级是X28级,后来结合电离层效应估计在X45级左右
2 McIntosh P S.The classification of sunspot groups.Solar Phys,1990,125:251–267
3 Wheatland M S.Rates of flaring in individual active regions.Solar Phys,2001,203:87–106
4 Giovanelli R G.The relations between eruptions and sunspots.Astrophys J,1939,89:555–567
5 Greatrix G R.On the statistical relations between flare intensity and sunspots.Mon Not Roy Astron Soc,1963,126:123–133
6 Kildahl K.In:Solar-Terrestrial Predictions Proceedings 3.Boulder Colorado:U S Dept Commerce,1980.166–166
7 Atac T.Statistical relationship between sunspots and major flares.Astrophys Space Sci,1987,129:203–208
8 Bornmann P L,Shaw D.Flare rates and the McIntosh active-region classifications.Solar Phys,1994,150:127–146
9 Sammis I,Tang F,Zirin H.The dependence of large flare occurrence on the magnetic structure of sunspots.Astrophys J,2000,540:583–587
10 Zhang H.Magnetic shear of a large delta sunspot group(NOAA 6659)in June 1991.Astron Astrophys,1995,297:869–880
11 Liu Y,Zhang H.Relationship between magnetic evolution and major flare event on July 14.Astron Astrophys,2001,372:1019–1029
12 Liu Y,Zhang H.Analysis of delta spot.Astron Astrophys,2002,386:646–652
13 Chumak O V,Chumak Z N.A stochastic method of describing the evolution of solar active regions(in Russian).Kinematika i Fizika Nebesnykh Tel,1987,3:7–13
14 Guo J,Zhang H Q,Chumak O V,et al.A quantitative study on magnetic configuration for active regions.Solar Phys,2006,237:25–43
15 Guo J,Zhang H Q,Chumak O V,et al.The evolution of the quantified magnetic complexity of active regions in the 23rd solar cycle.Mon Not R Astron Soc,2010,405:111–114
16 Cui Y M,Li R,Zhang L Y,et al.Correlation between solar flare productivity and photospheric magnetic field properties.Solar Phys,2006,237:45–59
17 Yang X,Zhang H Q,Gao Y,et al.A statistical study on photospheric magnetic nonpotentiality of active regions and its relationship with flares during solar cycles 22-23.Solar Phys,2012,280:165–181
18 Zirin H,Liggett M A.Delta spots and great flares.Solar Phys,1987,133:267–283
19 Jakimiec M,Paciorek J,Bartkowiak A.A multivariate comparison of delta and of other magnetic class sunspot groups.Acta Astron,1991,41:61–71
20 Shi Z,Wang J.Delta-sunspots and X-class flares.Solar Phys,1994,149:105–118
21 Achong A,Stahl P A.SID flare production is independent of Mt.Wilson magnetic class.Solar Phys,1984,92:259–269
22 Ternullo M,Contarino L,Romano P,et al.A statistical analysis of sunspot groups hosting M and X flares.Astron Nachr,2006,327:36–43
23 Kno ska S,Kr ivsky`L.Types of sunspots,magnetic classification and flare yield in cycle no.20.Bull Astron Inst Czech,1981,32:292–303
24 Chen A Q,Wang J X,Li J W,et al.Statistical properties of superactive regions during solar cycles 19-23.Astron Astrophys,2011,534:47–55
25 Gupta M,Mishra V K,Mishra A P.Solar activity parameters and their interrelationship:Continuous decrease in flare activity from solar cycles 20to 23.J Geophys Res,2007,112:A05105
26 Zharkov S I,Zharkova V V.Statistical properties of Hαflares in relation to sunspots and active regions in the cycle 23.J Atmosph Solar-Terrestrial Phys,2011,73:264–270
27 Zhang L Y,Cui Y M,He Y L,et al.Longitudinal distribution of major solar flares during 1975-2005.Adv Spa Res,2007,40:970–975
28 Leif Svalgaard L,Cliver E W,Kamide Y.Sunspot cycle 24:Smallest cycle in 100 years?Geophys Res Lett,2005,32(1):L01104
29 Bell B,Glazer H.Some sunspot and flare statistics.Smithsonian Contr Astrophys,1959,3:25–38
30 Feldman U,Doschek G A,Klimchuk J A.The occurrence rate of soft X-Ray flares as a function of solar activity.Astrophys J,1997,474:511–517
31 Yin S Y,Chen P F,Ding M D,et al.A statistical study of soft X-ray flares during solar cycle 22(in Chinese).J Nanjing Univ(Nat Sci),2002,38:458–461[尹素英,陈鹏飞,丁明德,等.第22太阳活动周软X射线耀斑的统计研究.南京大学学报(自然科学),2002,38:458–461]
32 Ternullo M,Zuccarello F,Contarino L,et al.A statistical approach to the spot-flare connection.In:the Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188.Netherlands:ESA Publications Division,2002.591–594
1)因为强度超过了探测器极限,根据外推得到的等级是X28级,后来结合电离层效应估计在X45级左右