On the Coronal Magnetic Field: Consequences of Large-Scale Motions

Details On the Coronal Magnetic Field: Consequences of Large-Scale Motions On the Coronal Magnetic Field: Consequences of Large-Scale Motions

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...521..868f&link_type=abstract

The Astrophysical Journal, Volume 521, Issue 2, pp. 868-877.

Astronomy and Astrophysics

Astronomy

78

Magnetohydrodynamics: Mhd, Sun: Solar Wind, Sun: Activity, Sun: Corona, Sun: Magnetic Fields

Scientific paper

A model has been introduced for the magnetic field in the heliosphere in which the field lines execute large excursions in heliographic latitude. The excursions result from the interplay between the differential rotation of the photosphere and the nonradial expansion of the solar wind near the Sun. The model accounts for the observed ease with which low-rigidity particles propagate in latitude in the solar wind. In this paper the consequences of this model for the behavior of the coronal magnetic field are explored. It is pointed out that the model provides an explanation for the time evolution and apparent rigid rotation of polar coronal holes and the differences between fast and slow solar wind.

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