Asymmetric flux loops in active regions. II

Details Asymmetric flux loops in active regions. II Asymmetric flux loops in active regions. II

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..127...51p&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 127, May 1990, p. 51-64. Research supported by the Royal Society and SERC.

Physics

27

Coronal Loops, Magnetic Flux, Solar Magnetic Field, Solar Rotation, Solar Wind, Sunspots, Approximation, Mathematical Models, Solar Physics

Scientific paper

Magnetic flux loops in the subphotospheric layers of the sun are seriously asymmetrical as a consequence of the drag force exerted on them, because of the different rotational rate of the surrounding plasma. In numerical models of stationary slender flux loops in the plane parallel approximation, it is shown that a serious tilt is both possible and probable. Observational facts strongly support the case for high asymmetry. The different stability of p and f spots may also be related to such an asymmetry. The tilts are very sensitive to the rotational profile and to the magnetic field structure. Nevertheless the characteristic maximal tilts can be tentatively estimated to be 20 deg for thin flux tubes and 5 deg for thick tubes. For two of the five observational consequences of such a tilt order-of-magnitude estimates of the effects are given. The estimates are in reasonable accord with observations.

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