Three-dimensional structure of the coronal magnetic field and the solar wind speed distribution projected on the photosphere in 1974

Details Three-dimensional structure of the coronal magnetic field and the solar wind speed distribution projected on the photosphere in 1974 Three-dimensional structure of the coronal magnetic field and the solar wind speed distribution projected on the photosphere in 1974

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....92.4339h&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, May 1, 1987, p. 4339-4348.

Astronomy and Astrophysics

Astronomy

19

Coronal Holes, Line Of Sight, Magnetic Field Configurations, Photosphere, Solar Magnetic Field, Wind Velocity, Astronomical Maps, Polar Regions

Scientific paper

Since the solar wind and coronal holes were relatively steady in 1974, the average distribution of the solar wind speed on the source surface and that of the line-of-sight component of the photospheric magnetic fields (B1) can be constructed, with fair accuracy, by the superposed epoch analysis. The three-dimensional structure of the coronal magnetic fields is then computed from this average map of B1 based on the potential model. The average distribution of the solar wind speed on the source surface, obtained from interplanetary scintillation observations, is then projected onto the photosphere along the open field lines in the corona. The high-speed regions thus projected are compared with the He I (1083 nm) coronal holes and are found to have a similar geometry. The slower speed regions on the source surface have a sinusoidal structure in heliographic latitude-longitude coordinates and are similar to the brightness distribution of the K corona and the structure of closed field line regions projected onto the photosphere.

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