Physics
Scientific paper
May 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991p%26ss...39..737e&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 39, May 1991, p. 737-744.
Physics
11
Solar Corona, Stellar Mass Ejection, Stellar Models, Stellar Structure, Coronal Loops, Dynamic Models, Magnetohydrodynamics, Solar Activity, Spatial Distribution
Scientific paper
This paper investigates a number of general properties of loop-shaped coronal mass ejections (CMEs). It is shown that at distances from 2.5 solar radii through 10 solar radii from the sun's center the motion of CME in the plane of sky can be visualized as the radial motion of a quasi-circular region in the antisunward direction with the velocity of the center of gravity = (Vp - V-perpendicular) and a simultaneous expansion with respect to this center with velocity V-perpendicular, with the quasi-circular shape remaining unchanged. At a certain distance (r greater than 2.5 solar radii) the relationship V-perpendicular/Vp - V-perpendicular = const begins to saturated. Using an improved variant of Webb's (1988) model it is shown that, according to its structure, the CME can be shaped both as a loop and as a shell and as a filled shell. With the obtained properties allowed for, the velocity V-perpendicular, of the CME's forefront is calculated, its mass and total kinetic energy E for cases where the motion of the CME occurs at an angle beta to the plane of sky.
Eselevich V. G.
Filippov M. A.
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