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

Content Provider	Springer Nature Link
Author	Eselevich, V. G. Eselevich, M. V.
Copyright Year	2015
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).
Starting Page	21
Ending Page	30
Page Count	10
File Format	PDF
ISSN	00109525
Journal	Cosmic Research
Volume Number	53
Issue Number	1
e-ISSN	16083075
Language	English
Publisher	Pleiades Publishing
Publisher Date	2015-02-01
Publisher Place	Moscow
Access Restriction	One Nation One Subscription (ONOS)
Subject Keyword	Astronomy, Astrophysics and Cosmology Astrophysics and Astroparticles Extraterrestrial Physics, Space Sciences
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Aerospace Engineering Space and Planetary Science

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