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Solar Physics

, Volume 282, Issue 2, pp 579–613 | Cite as

Solar Energetic Particle Events in the 23rd Solar Cycle: Interplanetary Magnetic Field Configuration and Statistical Relationship with Flares and CMEs

  • R. MitevaEmail author
  • K.-L. Klein
  • O. Malandraki
  • G. Dorrian
Article

Abstract

We study the influence of the large-scale interplanetary magnetic field configuration on the solar energetic particles (SEPs) as detected at different satellites near Earth and on the correlation of their peak intensities with the parent solar activity. We selected SEP events associated with X- and M-class flares at western longitudes, in order to ensure good magnetic connection to Earth. These events were classified into two categories according to the global interplanetary magnetic field (IMF) configuration present during the SEP propagation to 1 AU: standard solar wind or interplanetary coronal mass ejections (ICMEs). Our analysis shows that around 20 % of all particle events are detected when the spacecraft is immersed in an ICME. The correlation of the peak particle intensity with the projected speed of the SEP-associated coronal mass ejection is similar in the two IMF categories of proton and electron events, ≈ 0.6. The SEP events within ICMEs show stronger correlation between the peak proton intensity and the soft X-ray flux of the associated solar flare, with correlation coefficient r=0.67±0.13, compared to the SEP events propagating in the standard solar wind, r=0.36±0.13. The difference is more pronounced for near-relativistic electrons. The main reason for the different correlation behavior seems to be the larger spread of the flare longitude in the SEP sample detected in the solar wind as compared to SEP events within ICMEs. We discuss to what extent observational bias, different physical processes (particle injection, transport, etc.), and the IMF configuration can influence the relationship between SEPs and coronal activity.

Keywords

Coronal mass ejections, interplanetary Energetic particles Magnetic fields, interplanetary 

Notes

Acknowledgements

The authors acknowledge D. Boscher (ONERA Toulouse) for making the IPODE database of GOES particle measurements available to us. We also thank T. Dudok de Wit, M. Temmer, G. Trottet, H. Reid, and A. Veronig for helpful discussions and the referee for her/his comments. R.M. acknowledges a post-doctoral fellowship by Paris Observatory. The CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA.

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Copyright information

© Springer Science+Business Media Dordrecht 2012

Authors and Affiliations

  • R. Miteva
    • 1
    Email author
  • K.-L. Klein
    • 1
  • O. Malandraki
    • 2
  • G. Dorrian
    • 2
  1. 1.LESIA-Observatoire de ParisCNRS, UPMC Univ. Paris 06, Univ. Paris-DiderotMeudonFrance
  2. 2.Institute of Astronomy, Astrophysics, Space Applications and Remote SensingNational Observatory of AthensAthensGreece

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