Advertisement

Solar Physics

, Volume 233, Issue 1, pp 107–115 | Cite as

Comparison of the Variations of CMEs and ICMEs with those of other Solar and Interplanetary Parameters During Solar Cycle 23

  • R. P. KaneEmail author
Article

Abstract

This paper examines the variations of coronal mass ejections (CMEs) and interplanetary CMEs (ICMEs) during solar cycle 23 and compares these with those of several other indices. During cycle 23, solar and interplanetary parameters had an increase from 1996 (sunspot minimum) to ∼2000, but the interval 1998–2002 had short-term fluctuations. Sunspot numbers had peaks in 1998, 1999, 2000 (largest), 2001 (second largest), and 2002. Other solar indices had matching peaks, but the peak in 2000 was larger than the peak in 2001 only for a few indices, and smaller or equal for other solar indices. The solar open magnetic flux had very different characteristics for different solar latitudes. The high solar latitudes (45–90) in both N and S hemispheres had flux evolutions anti-parallel to sunspot activity. Fluxes in low solar latitudes (0–45) evolved roughly parallel to sunspot activity, but the finer structures (peaks etc. during sunspot maximum years) did not match with sunspot peaks. Also, the low latitude fluxes had considerable N–S asymmetry. For CMEs and ICMEs, there were increases similar to sunspots during 1996–2000, and during 2000–2002, there was good matching of peaks. But the peaks in 2000 and 2001 for CMEs and ICMEs had similar sizes, in contrast to the 2000 peak being greater than the 2001 peak for sunspots. Whereas ICMEs started decreasing from 2001 onwards, CMEs continued to remain high in 2002, probably due to extra contribution from high-latitude prominences, which had no equivalent interplanetary ICMEs or shocks. Cosmic ray intensity had features matching with those of sunspots during 2000–2001, with the 2000 peak (on a reverse scale, actually a cosmic ray decrease or trough) larger than the 2001 peak. However, cosmic ray decreases started with a delay and ended with a delay with respect to sunspot activity.

Keywords

Solar Cycle Coronal Mass Ejection Sunspot Number Sunspot Activity Sunspot Maximum 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Ataç, T. and Ozguç, A.: 1998, Solar Phys. 180, 397.CrossRefADSGoogle Scholar
  2. Cane, H. V., Richardson, I. G., and von Rosenvinge, T. T.: 1996, J. Geophys. Res. 101, 21561.ADSGoogle Scholar
  3. Cliver, E. W. and Hudson, H. S.: 2002, J. Atmos. Solar-Terres. Phys. 64, 231.ADSGoogle Scholar
  4. Gnevyshev, M. N.: 1967, Solar Phys. 1, 109.CrossRefADSGoogle Scholar
  5. Gopalswamy, N., Lara, A., Lepping, R. P., Kaiser, M. L., Berdichevsky, D., and St. Cyr, O. C.: 2000, Geophys. Res. Lett. 27, 145.ADSGoogle Scholar
  6. Gopalswamy, N., Lara, A., Yashiro, S., Kaiser, M. L., and Howard, R. A.: 2001, J. Geophys. Res. 106, 207.Google Scholar
  7. Gopalswamy, N., Lara, A., Yashiro, S., and Howard, R. A.: 2003a, Astrophys. J. 598, L63.CrossRefADSGoogle Scholar
  8. Gopalswamy, N., Lara, A., Yashiro, S., Nunes, S., and Howard, R. A.: 2003b, in Coronal Mass Ejection Activity During Solar Cycle 23, Proceedings of the ISCS 2003 Symposium, Solar Variability as an Input to the Earth's Environment, pp. 403–414, Tatranská Lomnica, Slovakia, ESA SP-535, September, 2003 (Ed. Wilson) ESTEC, Noordwijk, The Netherlands.Google Scholar
  9. Jokipii, J. R. and Thomas, B.: 1981, Astrophys. J. 243, 1115.CrossRefADSGoogle Scholar
  10. Kane, R. P.: 2005a, Solar Phys. 227, 155.CrossRefADSGoogle Scholar
  11. Kane, R. P.: 2005b, J. Atmos. Solar-Terr. Phys. 67, 429.ADSGoogle Scholar
  12. Kota, J. and Jokipii, J. R.: 1983, Astrophys. J. 265, 573.CrossRefADSGoogle Scholar
  13. Munro, R. H., Gosling, J. T., Hildner, E., MacQueen, R. M., Poland, A. I., and Ross, C. L.: 1979, Solar Phys. 61, 201.CrossRefADSGoogle Scholar
  14. Rybansky, M., Rusin, V., and Minarovjech, M.: 1998, Solar Phys. 177, 305.ADSGoogle Scholar
  15. St. Cyr, O. C., Howard, R. A., Sheeley, N. R. et al.: 2000, Properties of coronal mass ejections: SOHO LASCO observations from January 1996 to June 1998, J. Geophys. Res. 105, 18169.CrossRefADSGoogle Scholar
  16. Tousey, R.: 1973, in M. J. Rycroft and S. K. Runcom (eds.), The Solar Corona, Springer-Verlag, New York, p. 173.Google Scholar
  17. Vernova, E. S., Mursula, K., Tyasto, M. I., and Baranov, D. G.: 2002, Solar Phys. 205, 371.CrossRefADSGoogle Scholar
  18. Wang, Y.-M. and Sheeley, N. R.: 2002, J. Geophys. Res. 107, 1302, doi:10.1029/2001JA000500.Google Scholar
  19. Webb, D. F. and Howard, R. A.: 1994, J. Geophys. Res. 99, 4201.CrossRefADSGoogle Scholar
  20. Woods, T. N., Tobiska, W. K., Rottman, G. J., and Worden, J. R.: 2000, J. Geophys. Res. 105, 27195.CrossRefADSGoogle Scholar

Copyright information

© Springer Science + Business Media, Inc. 2006

Authors and Affiliations

  1. 1.Instituto Nacional de Pesquisas Espaciais, INPESão PauloBrazil

Personalised recommendations