Non-radial motion of eruptive filaments

Details Non-radial motion of eruptive filaments Non-radial motion of eruptive filaments

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001soph..203..119f&link_type=abstract

Solar Physics, v. 203, Issue 1, p. 119-130 (2001).

Physics

25

Scientific paper

We develop a simple model to explain the non-radial motion of eruptive solar filaments under solar minimum conditions. The global magnetic field is derived from the first and third components of the spherical harmonic expansion of a magnetic scalar potential. The filament is modeled as a toroidal current located above the mid-latitude polarity inversion line. We investigate the stability of the filament against changes in the filament current and attempt to explain the non-radial motion and acceleration of the eruptive filament. We also discuss the limitations of this model.

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