Martens-Kuin models of normal and inverse polarity filament eruptions and coronal mass ejections

Details Martens-Kuin models of normal and inverse polarity filament eruptions and coronal mass ejections Martens-Kuin models of normal and inverse polarity filament eruptions and coronal mass ejections

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..137..317s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 137, Feb. 1992, p. 317-328.

Physics

8

Atmospheric Models, Magnetic Field Configurations, Solar Atmosphere, Solar Corona, Solar Magnetic Field, Solar Prominences, Magnetic Flux, Magnetohydrodynamic Flow, Polarity

Scientific paper

An analysis is made of the Martens-Kuin filament eruption model in relation to observations of coronal mass ejections (CMEs). The field lines of this model are plotted in the vacuum or infinite resistivity approximation with two background fields. The first is the dipole background field of the model and the second is the potential streamer model of Low. The Martens-Kuin model predicts that, as the filament erupts, the overlying coronal magnetic field lines rise in a manner inconsistent with observations of CMEs associated with eruptive filaments. This model and, by generalization the whole class of so-called Kuperus-Raadu configurations in which a neutral point occurs below the filament, are of questionable utility for CME modeling. An alternate case is considered in which the directions of currents in the Martens-Kuin model are reversed resulting in a so-called normal polarity configuration of the filament magnetic field. The background field lines now distort to support the filament and help eject it. While the vacuum field results make this configuration appear very promising, a full two- or more-dimensional MHD simulations is required to properly analyze the dynamics resulting from this configuration.

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