The coronal field lines of an evolving bipolar magnetic region

Details The coronal field lines of an evolving bipolar magnetic region The coronal field lines of an evolving bipolar magnetic region

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...255..316s&link_type=abstract

Astrophysical Journal, Part 1, vol. 255, Apr. 1, 1982, p. 316-319.

Astronomy and Astrophysics

Astrophysics

6

Coronal Loops, Magnetic Flux, Photosphere, Solar Magnetic Field, Magnetohydrodynamics, Point Sources, Potential Fields, Solar Rotation, Solar Wind, Stellar Models

Scientific paper

A simple potential field model is presented to illustrate that loops of magnetic flux rise upward through the corona during the relatively short growth phase of a bipolar magnetic region but contract back to the sun's surface during the much longer decay phase of the photospheric region. To reconcile this behavior with the unidirectional, solar-wind-driven convection of flux outward from the sun, one must postulate the existence of an X-type neutral line in the middle corona where open field lines can be converted back to closed ones.

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