General solution for interplanetary magnetic field produced from stationary sources on the sun

Details General solution for interplanetary magnetic field produced from stationary sources on the sun General solution for interplanetary magnetic field produced from stationary sources on the sun

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986p%26ss...34.1299n&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 34, Dec. 1986, p. 1299-1305.

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Interplanetary Magnetic Fields, Magnetic Field Configurations, Solar Wind Velocity, Polar Coordinates, Vortices

Scientific paper

It is well known that interplanetary space contains Parker's (1958) Archimedean spiral magnetic field, the components of which are respectively radial and longitudinal in the solar polar coordinates (r, theta, phi) and are intimately related to each other, depending on the solar wind velocity. In this paper, a general solution of the interplanetary magnetic field which is produced from time-independent sources fixed on the solar surface and contains the Parker field as a particular solution is presented. The field is first classified broadly into two types called the phi-dependent (or nonzonal) and the phi-independent (or zonal) fields. The former field is further subdivided into two types, one is the so-called Parker type, and the other is the vortex type which has no radial component. The resultant of these two fields exhibits the helical (or twisted) structure in space, tentatively introduced by Lee and Fisk (1981). The zonal field is also subclassified into two; one is the radial-type zonal field, and the other is the toroidal field. These two fields are mutually independent, and therefore their resultant does not always coincide in direction with the Parker field.

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