Magnetic field re-arrangement after prominence eruption

Details Magnetic field re-arrangement after prominence eruption Magnetic field re-arrangement after prominence eruption

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..235k&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 235-239 (SEE N87-20871 13-92)

Mathematics

1

Coronal Holes, Solar Corona, Solar Flares, Solar Magnetic Field, Solar Prominences, Magnetic Field Configurations, Mathematical Models, Sun

Scientific paper

It has long been known that magnetic reconnection plays a fundamental role in a variety of solar events. Although mainly invoked in flare problems, large scale loops interconnecting active regions, evolving coronal hole boundaries, the solar magnetic cycle itself, provide different evidence of phenomena which involve magnetic reconnection. A further example might be given by the magnetic field rearrangement which occurs after the eruption of a prominence. Since most often a prominence reforms after its disappearance and may be observed at about the same position it occupied before erupting, the magnetic field has to undergo a temporary disruption of relax back, via reconnection, to a configuration similar to the previous one. The above sequence of events is best observable in the case of two ribbon (2-R) flares but most probably is associated with all filament eruptions. Even if the explanation of the magnetic field rearrangement after 2-R flares in terms of reconnection is generally accepted, the lack of a 3-dimensional model capable of describing the field reconfiguration, has prevented, up to now, a thorough analysis of its topology as traced by H alpha/x ray loops. A numerical technique is presented which enables oneto predict and visualize the reconnected configuration, at any time, and therefore allows one to make a significant comparison of observations and model predictions throughout the whole process.

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