Abstract
The signatures of the geoeffectiveness solar disturbed events on the Magnetosphere Convection Electric Field (MCEF) universal time variation from 1964 to 2009 are investigated. Here, attention is focused our on the periods concerned by the whole shock activity and by the different types of the geoeffectiveness Coronal Mass Ejections (CMEs) which are one-day-shock, two-days-shock and three-days-shock. The investigation is made with respect to the orientation of the Interplanetary Magnetic Field (IMF). The MCEF time profiles show three different trends except for one-day-shock activity and for three-days-shock activity where we have four trends and one trend, respectively. The MCEF time profiles of the whole disturbed activity, the all shock activity and the one-day-shock activity present the initial phase where the Interplanetary Magnetic Field (IMF) is southward. During the two-days-shock activity, the initial phase of the MCEF shows a non-sensitive trend to the change of the direction of the IMF z-component while for the three-days-shock activity, the MCEF always exhibits the signature of the northward IMF. The last trend of the MCEF time profile shows the southward IMF signature except for the one-day-shock and the three-days-shock activities where that of the northward IMF was seen. Key words: Magnetosphere convection electric field, interplanetary magnetic field, shock activity, coronal mass ejections (CMEs).  
Highlights
The magnetosphere created by the solar wind is a very sensitive and dynamic entity (Russel, 1979) a behaviour that depends on the properties of the solar wind plasma and its frozen magnetic field (Mc Pherron et al, 2007)
After analysing the Universal Time (UT) variation of the Earth Magnetosphere Convection Electric Field (MCEF) under the shock conditions, we focus our attention on the UT variation of the Earth MCEF during each type of the shock activity
The present work shows that the mean amplitudes of the MCEF during the whole disturbed period are inferior to those of the shock activity period
Summary
The magnetosphere created by the solar wind is a very sensitive and dynamic entity (Russel, 1979) a behaviour that depends on the properties of the solar wind plasma and its frozen magnetic field (Mc Pherron et al, 2007). According to Mc Pherron et al (2007), there are three possible magnetic topologies during the interaction between the solar wind and the planetary magnetosphere. We can cite the topology where a magnetic line might not intersect the Earth at all and that where a magnetic line might intersect the surface of the Earth.
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