Volume 33 Issue 3
May  2013
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Article Navigation >  Chinese Journal of Space Science  > 2013  >  33(3): 225-230
Meng Weijuan, Le Guiming, Lin Zhaoxiang, Zhang Yong, Yang Xingxing. Distribution of CMEs in different angular width and its relationship with the phase of sunspot numbers in solar cycle 23[J]. Chinese Journal of Space Science, 2013, 33(3): 225-230. doi: 10.11728/cjss2013.03.225
Citation: Meng Weijuan, Le Guiming, Lin Zhaoxiang, Zhang Yong, Yang Xingxing. Distribution of CMEs in different angular width and its relationship with the phase of sunspot numbers in solar cycle 23[J]. Chinese Journal of Space Science, 2013, 33(3): 225-230. doi: 10.11728/cjss2013.03.225
shu

Distribution of CMEs in different angular width and its relationship with the phase of sunspot numbers in solar cycle 23

doi: 10.11728/cjss2013.03.225 cstr: 32142.14.cjss2013.03.225
  • 1.

    South-Center University for Nationalities, Wuhan 430074

  • 2.

    National Satellite Meteorology Center for Space Weather, CMA, Beijing 100081

  • 3.

    Nanjing University of Information Science and Technology, Nanjing 210044

  • Received Date: 2012-12-03
  • Rev Recd Date: 2013-02-17
  • Publish Date: 2013-05-15
    Abstract
  • In this paper we statistically analyzed the distribution of the numbers of CME with different angle width during the period of 1996-2008. Then we obtained the relationship between the number of CME with some typical angle width varying with time and that the sunspot numbers varying with time. The analytical results indicate that the numbers of CME within angle width 0° ～ 180° make up 95%, full-halo CMEs make up 2.83%, and the quantities of CME within angle width 301° ～ 359° make up very little proportion of all CMEs. The CMEs of angle width 0° ～ 60° have three peaks, which doesn't match the characteristics of sunspot numbers varying with time. There is no two-peak distribution of the numbers of CME within angle width 121° ～ 180°. Moreover, the distribution of full-halo CMEs has a typical two-peak structure, with the first peak appearing in 2001 and the second peak appearing in 2005, which is not synchronized with the distribution of sunspot numbers.

     

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