Formation and Development of Shock Waves in the Solar Corona and Near-Sun Interplanetary Space and Solar Energetic Particle Events

Details Formation and Development of Shock Waves in the Solar Corona and Near-Sun Interplanetary Space and Solar Energetic Particle Events Formation and Development of Shock Waves in the Solar Corona and Near-Sun Interplanetary Space and Solar Energetic Particle Events

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh21b..03m&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH21B-03

Physics

7509 Corona, 7513 Coronal Mass Ejections, 7514 Energetic Particles (2114), 7851 Shock Waves

Scientific paper

At the Sun shock waves are produced either by flares or by coronal mass ejections and are regarded as the source of solar energetic particle events. In the corona shock waves appear as solar type II radio bursts often associated with coronal transient (or EIT) waves. The propagation of a disturbance through the corona away from an active region into the interplanetary space is considered by evaluating the radial behaviour of the Alfven speed. The magnetic field of an active region is modelled by a magnetic dipole and is superimposed on that of the quiet Sun as deduced from the EIT wave analysis. Such a behaviour of the magnetic field leads to a local minimum of the Alfven speed in the range 1.2-1.8 solar radii in the corona as well as a maximum of 740 km/2 at a distance of 3.8 solar radii. The occurrence of such a minimum and maximum of the Alfven speed has important consequences to the formation and development of shock waves in the corona and near-Sun interplanetary space and to their ability to accelerate particles leading to a special temporal behaviour of solar energetic particle events.

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