Characteristics of coronal mass ejections associated with interplanetary shocks

Details Characteristics of coronal mass ejections associated with interplanetary shocks Characteristics of coronal mass ejections associated with interplanetary shocks

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..151..333b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 151, no. 2, p. 333-339

Physics

6

Flux Transfer Events, Interplanetary Medium, Shock Wave Interaction, Solar Corona, Solar Wind, Classifications, Coronagraphs, Dynamic Characteristics, Magnetohydrodynamic Turbulence, Mass Distribution, Plasma Loss, Surveys

Scientific paper

In a correlated study using coronagraph and interplanetary from 1978 to 1983, a set of 56 coronal mass ejections (CMEs) was confidently associated with interplanetary shocks by Sheeley et al. (1985). In this paper we analyze the characteristics of these particular CMEs in contrast to the whole population of them during the period. We find that the associated CMEs are not a representative sample of all the variety of CMEs and that they share specific characteristics. Contrary to common beliefs, these characteristics are not a high velocity or a large extension, but have more to do with the importance and shape of the CME. Practically all the CMEs associated with shocks were of importance Y (bright and/or large) and had a curved-type front structural class (a continuous curved front with either straight edges or curved legs). Another common characteristic of these particular CMEs is that they show a considerable increase in their angular span as they go out from the Sun, moving the peak of the distribution from approximately equal 30 deg to approximately equal 70 deg.

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