On the structure of the distant magnetotail - ISEE 3

Details On the structure of the distant magnetotail - ISEE 3 On the structure of the distant magnetotail - ISEE 3

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....97.1403f&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, Feb. 1, 1992, p. 1403-1410.

Physics

27

Earth Magnetosphere, Geomagnetic Tail, International Sun Earth Explorer 3, Magnetosheath, Earth Planetary Structure, Satellite Observation, Solar Wind

Scientific paper

The relative frequency of observation of the magnetosheath and magnetotail in the region where a nominal magnetotail is expected is determined on the basis of ISEE-3 magnetic field and electron plasma data. These observations are compared with how frequently a tail of a given radius would be expected to be seen, assuming typical variations in the direction of the solar wind flow relative to the radial. Observations match expectations if the average radius consistent with an open magnetotail where field lines are lost both through the magnetopause and also by closing along the equatorial current sheet. This relatively small radius is consistent with an open magnetotail where field lines are lost both through the magnetopause and also by closing across the equatorial current sheet. The average solar magnetospheric Bz component of the field in the distant plasma sheet is 0.6 nT during quiet times but zero during disturbed times, which suggests that when the polar cap becomes smaller during quiet times, many of the field lines that previously formed the distant tail lobes are converted into closed field lines that cross the equatorial plane earthward of 240 RE.

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