Modeling Vertical Plasma Flows in Solar Filament Barbs

Details Modeling Vertical Plasma Flows in Solar Filament Barbs Modeling Vertical Plasma Flows in Solar Filament Barbs

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh22a0184l&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH22A-0184

Physics

7507 Chromosphere, 7509 Corona, 7524 Magnetic Fields

Scientific paper

Speeds of observed flows in quiescent solar filaments are typically much less than the local Alfvén speed. This is why the flows in filament barbs can be modeled by perturbing a local magnetostatic solution describing the balance between the Lorentz force, gravity, and gas pressure in a barb. Similarly, large-scale filament flows can be treated as adiabatically slow deformations of a force-free magnetic equilibrium that describes the global structure of a filament. This approach reconciles current theoretical models with the puzzling observational result that some of the flows appear to be neither aligned with the magnetic field nor controlled by gravity.

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