Physics
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993georl..20.2695p&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 20, no. 23, p. 2695-2698
Physics
39
Geomagnetic Tail, Interplanetary Magnetic Fields, Mathematical Models, Shapes, Size (Dimensions), Angles (Geometry), Boundaries, International Sun Earth Explorer 1, Solar Wind
Scientific paper
A model of the size and shape of the near-earth magnetotail which depends upon distance downtail, rho V(exp 2)(sub SW), and Interplanetary Magnetic Field (IMF) B(sub z) has been developed. This empirical model was developed by first using observations of the magnetic field in the lobe by International Sun Earth Explorer-1 (ISEE-1) and simultaneous observations of the magnetic field and plasma properties of the solar wind by IMP-8 to determine the flaring angle of the near-earth magnetotail in the region -22.5 R(sub e) less than or equal to x less than or equal to -10R(sub e). These studies show that the flaring angle depends on x, rho V(exp 2)(sub SW), and IMF B(sub z). In particular, the median flare angle increases linearly with decreasing B(sub z) when the IMF is southward, while the flare angle is constant when the IMF is northward. The empirical function derived for the flaring angle of the magnetotail is used to determine a relation for the radius of the tail.
Petrinec Steven M.
Russell Christopher T.
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