Expansion and broadening of coronal loop transients - A theoretical explanation

Details Expansion and broadening of coronal loop transients - A theoretical explanation Expansion and broadening of coronal loop transients - A theoretical explanation

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..675m&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 675-682.

Astronomy and Astrophysics

Astrophysics

86

Loops, Solar Corona, Solar Magnetic Field, Stellar Models, Coronagraphs, Drag, Lines Of Force, Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamic Stability

Scientific paper

Consequences are examined of the assumption that an observed coronal loop transient is a twisted rope of magnetic-field lines expanding and broadening in the background coronal plasma and magnetic field. It is shown that the expansion can be accounted for by the azimuthal component of the field; the observed broadening of the loop as it moves outward can be accounted for by the longitudinal component of the field. In order to have a net outward force and at the same time avoid a classical pinch (sausage) instability, the two components of the field must satisfy a certain inequality. It is predicted that, as the loop rises, the width (h) of its top portion should vary proportionally with distance (R) from the sun's center. This is in good agreement with measurements that show h is proportional to the 0.8 power of R. The prediction that the radius of curvature of the top portion of the loop should be proportional to R differs from the measured variation. The difference could be accounted for by a drag due to the background coronal field that flattens the loop's top.

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