Dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. VI - Small flux bundles, network fields, and ephemeral active regions

Details Dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. VI - Small flux bundles, network fields, and ephemeral active regions Dynamical oscillation and propulsion of magnetic fields in the convective zone of a star. VI - Small flux bundles, network fields, and ephemeral active regions

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...326..407p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 1, 1988, p. 407-411.

Astronomy and Astrophysics

Astrophysics

8

Scientific paper

Simple analysis of the hydrodynamics initiated by the presence of a coherent flux bundle in the lower half of the convective zone of a star like the Sun indicates that bundles with diameters comparable to the local pressure scale height (5 x 10 cm) are subject to sidewise motions perhaps as fast as 10 cm 51 The motions arise as a consequence of the bundle being squeezed between the cool shadow above and the accumulating heat below, and because of convective propulsion. This suggests that the equatorward motion (102 cm s1) of the azimuthal fields, inferred from observations of the Sun, may be as much a consequence of the hydrodynamics of flux bundles and meridional circulation as it is of the dynamo effects that create the flux. Subject headings: hydromagnetics - stars: interiors stars: magnetic

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