Computer Science
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..125r&link_type=abstract
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 125-1
Computer Science
Particle Emission, Solar Wind, Interplanetary Magnetic Fields
Scientific paper
Most inversions of the structure of magnetic ropes in ICMEs have assumed that the rope can be approximated as a force-free structure in the Taylor state in which the current is not only parallel to the magnetic field but everywhere has the same constant of proportionality to the field strength. The solution of this problem is a magnetic field that is describable by Bessel functions: Jo for the axial component and J1 for the poloidal component. The Taylor state approximation has a maximum twist that is exceeded by about half the observed flux ropes. Moreover, many flux ropes are not force-free. The vast majority of non-force-free ropes have an excess of pressure pushing outward. Thus these ropes are either expanding or are balanced by non-magnetic forces. Thus while the Bessel function approach may be useful for determining the orientation of rope axes, its limited ability to correctly measure twist and its inability to assess any magnetic force imbalance mitigate against its usefulness in studies of ICME genesis and evolution.
Mulligan T.
Russell Christopher T.
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