Understanding the large-scale structure of magnetic fields in the corona and heliosphere

Details Understanding the large-scale structure of magnetic fields in the corona and heliosphere Understanding the large-scale structure of magnetic fields in the corona and heliosphere

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...91z&link_type=abstract

Stanford Univ., International Solar Wind 8 Conference, p. 91

Other

Coronas, Heliosphere, Interplanetary Magnetic Fields, Photosphere, Astronomical Models, Stellar Activity, Current Sheets, Magnetic Flux, Planetary Magnetic Fields, Ulysses Mission, Interplanetary Space

Scientific paper

To understand the non-radial nature of the southwestern streamer in the 3 November 1994 eclipse and the near absence of a latitudinal gradient of the interplanetary magnetic field strength seen by Ulysses over the southern pole, we calculate the coronal and inter planetary magnetic field from WSO photospheric field data using both the horizontal current-current sheet model (Zhao and Hoeksema, 1994) and the current sheet-source surface model (Zhao and Hoeksema, 1995). These models account for the effects of large-currents and current sheets in the corona. Comparison of the calculated results with white light, X-ray, and IMF observations show that non-radial coronal streamers and a near-zero latitudinal gradient of the radial component of the IMF may be explained by a large-scale current sheet. To best match the observations, the height of the cusp point (above which current sheets form) differs from one streamer to another. While heliospheric volume currents flowing above the source surface certainly affect the interplanetary field, they have little or no influence on the structure of the corona.

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