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Differences in the development of the initial phase of the formation of two types of coronal mass ejections

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Abstract

Based on the results of an analysis of AIA/SDO and EUVI/STEREO data it was confirmed that the initial phase of the “gradual” coronal mass ejection (CME) begins as a motion from the rest of the outer shell of a coronal magnetic rope, which then becomes the basis of the frontal structure of a CME. It is shown by an example of an analysis of an event on January 5, 2013 that a different type of CME, “impulsive,” can occur as a result of the ejection of a “cavity” from the lower solar corona (the 193 Å channel), which then becomes the basis for future CME. An analysis of the three-dimensional structure of the cavity, its dynamics and kinematics, as well as a comparison of the results of an analysis with numerical calculations allow us to interpret observations as a manifestation of the rapid rise of the magnetic tube (rope) filled with cold plasma. The appearance of the rope in the lower corona probably is a result of its rapid floating (with supersonic velocity) from the solar convective zone. Theoretical estimates show that the cause of the ejection of the magnetic tube from the convective zone can be the development of a Parker’s instability (“slow” wave).

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Authors and Affiliations

  1. Institute of Solar-Terrestrial Physics, Siberian Branch, Russian Academy of Sciences, Irkutsk, 664033, Russia

    V. G. Eselevich & M. V. Eselevich

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  1. V. G. Eselevich
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  2. M. V. Eselevich
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Correspondence to V. G. Eselevich.

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Original Russian Text © V.G. Eselevich, M.V. Eselevich, 2015, published in Kosmicheskie Issledovaniya, 2015, Vol. 53, No. 1, pp. 24–34.

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Eselevich, V.G., Eselevich, M.V. Differences in the development of the initial phase of the formation of two types of coronal mass ejections. Cosmic Res 53, 21–30 (2015). https://doi.org/10.1134/S0010952515010049

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