Abstract
During an eruptive flare a large magnetic loop or plasmoid is ejected into interplanetary space, and the closed magnetic field structure which exists prior to the flare becomes opened. One of the requirements of flare models is to explain how the field can be opened while decreasing the overall magnetic energy of the system. After the field is opened, reconnection must occur in order to restore the field to its pre-flare configuration. The strongest evidence for reconnection in flares comes from observations of the chromospheric ribbons and the coronal loops which form after the onset of a large flare. The ribbons and loops appear to propagate through the chromosphere and corona during the flare, but Doppler-shift measurements show conclusively that these apparent motions are not due to mass motions of the solar plasma. The motions can only be explained by the upward propagation of an energy source in the corona, and in the 1VIHD-reconnection model of flares, the propagating energy source is an x-line accompanied by slow-mode shocks.
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© 1992 Springer-Verlag
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Forbes, T.G. (1992). Field opening and reconnection. In: Švestka, Z., Jackson, B.V., Machado, M.E. (eds) Eruptive Solar Flares. Lecture Notes in Physics, vol 399. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-55246-4_80
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DOI: https://doi.org/10.1007/3-540-55246-4_80
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