Statistics of sunspot group clusters

Journal of Space Weather and Space Climate

Ryszarda Getko¹ 

[1] Astronomical Institute, University of Wrocław,Kopernika 11,51–622 Wrocław,Poland

关键词: variability;    statistics and probability;    sunspot;    Sun;   

Others  :  800631
DOI  :  doi:10.1051/swsc/2013032

 received in 2012-02-27, accepted in 2013-02-16,  发布年份 2013

【 摘 要 】

The Zubrzycki method is utilized to find all sunspot groups which are close to each other during each Carrington rotation. The sunspot group areas and their positions for the years 1874–2008 are used. The descending, the ascending and the maximum phases of solar cycles for each solar hemisphere are considered separately. To establish the size of the region D where the clusters are searched, the correlation function dependent on the distance between two groups is applied. The method estimates the weighted area of each cluster. The weights dependent on the correlation function of distances between sunspot groups created each cluster. For each cluster the weighted position is also evaluated. The weights dependent on the areas of sunspot groups created a given cluster. The number distribution of the sunspot groups created each cluster and the cluster statistics within different phases of the 11-year cycle and within all considered solar cycles are also presented.

【 授权许可】

   
© R. Getko, Published by EDP Sciences 2013

【 图 表 】

Fig. 1.

Fig. 2.

Fig. 3.

Fig. 4.

Fig. 5.

Fig. 6.

Fig. 7.

Fig. 8.

【 参考文献 】

• [1]Bogdan, T.J., P.A. Gilman, I. Lerche, and R. Howard, Distribution of sunspot umbral areas – 1917–1982, Astrophys. J., 327, 451–456, 1988. [NASA ADS]
• [2]Brouwer, M. P., and C. Zwaan, Sunspot nests as traced by a cluster analysis, Sol. Phys., 129, 221–246, 1990. [NASA ADS]
• [3]Castenmiller, M.J.M., C. Zwaan, and E.B.J. van der Zalm, Sunspot nests – Manifestations of sequences in magnetic activity, Sol. Phys., 105, 237–255, 1986. [NASA ADS]
• [4]Gaizauskas, V., K.L. Harvey, J.W. Harvey, and C. Zwaan, Large-scale patterns formed by solar active regions during the ascending phase of cycle 21, Astrophys. J., 265, 1056–1065, 1983. [NASA ADS]
• [5]Getko, R., Activity complexes as a cause of strong positive monthly Wolf number fluctuations, Sol. Phys., 224, 291–301, 2004.
• [6]Harvey, K.L., Magnetic bipoles on the Sun, PhD thesis. Utrecht University, 1993.
• [7]Harvey, K.L., and C. Zwaan, Properties and emergence of bipolar active regions, Sol. Phys., 148, 85–117, 1993. [NASA ADS]
• [8]Parnell, C.E., C.E. DeForest, H.J. Hagenaar, B.A. Johnston, D.A. Lamb, et al., A Power-law distribution of solar magnetic fields over more than five decades in flux, Astrophys. J., 69, 75–82, 2009. [NASA ADS]
• [9]Schrijver, C.J., Radiative fluxes from the outer atmosphere of a star like the Sun – A construction kit, A&A, 189, 163–172, 1988.
• [10]Schrijver, C.J., and K.L. Harvey, The photospheric magnetic flux budget, Sol. Phys., 150, 1–18, 1994. [NASA ADS]
• [11]Tang, F., R. Howard, and J.M. Adkins, A statistical study of active regions 1967–1981, Sol. Phys., 91, 75–86, 1984.
• [12]van Driel-Gesztelyi, L., E.B.J. van der Zalm, and C. Zwaan, Active nests on the Sun, Proc. of the National Solar Observatory/Sacramento Peak 12th Summer Workshop, ASP Conference Series, ASP, San Francisco, 27, 89, 1992.
• [13]Zubrzycki, S., About an estimation of the parameters of geological deposits, Wiadomosci matem., III, 105–153, 1957.