Laboratory simulations of solar prominence eruptions

Details Laboratory simulations of solar prominence eruptions Laboratory simulations of solar prominence eruptions

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phpl....5.1991b&link_type=abstract

Physics of Plasmas, Volume 5, Issue 5, pp. 1991-2000 (1998).

Physics

26

Plasma Simulation, Magnetic Confinement And Equilibrium

Scientific paper

Spheromak technology is exploited to create laboratory simulations of solar prominence eruptions. It is found that the initial simulated prominences are arched, but then bifurcate into twisted secondary structures which appear to follow fringing field lines. A simple model explains many of these topological features in terms of the trajectories of field lines associated with relaxed states, i.e., states satisfying ∇×B=λB. This model indicates that the field line concept is more fundamental than the flux tube concept because a field line can always be defined by specifying a starting point whereas attempting to define a flux tube by specifying a starting cross section typically works only if λ is small. The model also shows that, at least for plasma evolving through a sequence of force-free states, the oft-used line-tying concept is in error. Contrary to the predictions of line-tying, direct integration of field line trajectories shows explicitly that when λ is varied, both ends of field lines intersecting a flux-conserving plane do not remain anchored to fixed points in that plane. Finally, a simple explanation is provided for the S-shaped magnetic structures often seen on the sun; the S shape is shown to be an automatic consequence of field line arching and the parallelism between magnetic field and current density for force-free states.

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