Slow twists of solar magnetic flux tubes and the polar magnetic field of the sun

Details Slow twists of solar magnetic flux tubes and the polar magnetic field of the sun Slow twists of solar magnetic flux tubes and the polar magnetic field of the sun

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989georl..16..919h&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 16, Aug. 1989, p. 919-922.

Physics

36

Magnetic Flux, Magnetohydrodynamic Waves, Poynting Theorem, Solar Flux, Solar Magnetic Field, Solar Wind, Galactic Cosmic Rays, Solar Corona, Solar Rotation

Scientific paper

The solar wind model of Weber and Davis (1967) is generalized to compute the heliospheric magnetic field resulting from solar rotation or a steady axisymmetric twist including a geometrical expansion which is more rapid than spherical. The calculated increase in the ratio of the toroidal to poloidal field components with heliocentric radial distance r clarifies an expression derived recently by Jokipii and Kota (1989). Magnetic-field components transverse to r do not in general grow to dominate the radial component at large r. The analysis also yields expressions for the Poynting flux associated with the steady twists.

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