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Magnetic field re-arrangement after prominence eruptionIt 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.
Document ID
19870011474
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Kopp, R. A. (Los Alamos National Lab. NM, United States)
Poletto, G. (Florence Univ. Italy)
Date Acquired
September 5, 2013
Publication Date
December 1, 1986
Publication Information
Publication: NASA. Goddard Space Flight Center Coronal and Prominence Plasmas
Subject Category
Solar Physics
Accession Number
87N20907
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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