Solar and heliospheric origins of geomagnetic perturbations in the rising phase of Solar Cycle 23

Mathematics – Logic

Scientific paper

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Geomagnetic Perturbations, Heliosphere

Scientific paper

Solar sources of strong geomagnetic perturbations are connected to coronal mass ejections and corotating inhomogeneities in the heliosphere. Geomagnetic perturbations with Ap > 20 in 1997-2000 were produced by heliospheric magnetic fields and solar wind plasma streams related to the following morphological features observed at the Sun: 1) active and disappearing filaments and prominences (sdf) seen in Hα synoptic maps; 2) solar flares; 3) evolving active regions and coronal holes (CH); 4) heliospheric current sheet (HCS) positions deduced from photospheric magnetic field measurements. Strong geomagnetic storms during this period of time were observed when compound plasma streams from several sources on the Sun reached the Earth's magnetosphere. The combination of the transient processes and corotating inhomogeneities in the solar corona and deeper layers of the solar atmosphere not far from the center of the solar disk (first tens of degrees) represent a sufficient condition for the formation of such compound streams exemplified by sdf-CH-HCS passage.

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