Impulses of Coronal Activity and Their Relation to the Solar Cycle

Mathematics – Logic

Scientific paper

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7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7544 Stellar Interiors And Dynamo Theory, 7549 Ultraviolet Emissions

Scientific paper

SOHO/EIT Extreme Ultraviolet and YOHKOH soft X-ray data have revealed the close relation between the coronal structures and the photospheric magnetic flux. These data can be considered as a proxy of magnetic field structures in the corona. During the beginning of the solar cycle the evolution of the coronal structures and, therefore, the topological changes of the magnetic field reveal a quasiperiodical process of 'impulses of coronal activity' with a period of approximately 1-1.5 years. This process is represented by the evolution of giant coronal loops of hot plasma (2-3 MK), or by closed lines of magnetic field, which connect the following parts of the complexes of the sunspot activity with the solar polar regions (predominantly of the opposite polarity). The 'impulses of coronal activity' are correlated with the erupted magnetic flux in the mid-latitudinal zones, and they display non-uniform distributions with longitude. Therefore, the 'impulses' mostly reflect the non-axisymmetrical component of the solar magnetic field. The quasiperiodic behavior of the 'impulses' results from the characteristic lifetime and reappearance of the sunspot complexes in active longitudinal zones (active longitudes). We discuss the physical nature of the 'impulses of coronal activity' and their possible relations to the dynamo process.

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