Heating of coronal arcades by magnetic tearing turbulence, using the Taylor-Heyvaerts hypothesis

Details Heating of coronal arcades by magnetic tearing turbulence, using the Taylor-Heyvaerts hypothesis Heating of coronal arcades by magnetic tearing turbulence, using the Taylor-Heyvaerts hypothesis

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159..129b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 159, no. 1-2, April 1986, p. 129-141. SERC-supported research.

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Atmospheric Turbulence, Magnetic Field Reconnection, Plasma Heating, Solar Corona, Taylor Series, Computational Astrophysics, Solar Physics

Scientific paper

The heating of the solar corona by direct currents, which are dissipated by magnetic reconnection, is studied. The coronal field responds to slow photospheric motions by evolving through a series of equilibria, which may be unstable to resistive modes. According to a generalization of Taylor's hypothesis (Heyvaerts and Priest, 1984), the field reconnects and relaxes to a linear force-free state (satisfying Delta X B = alpha B), where the parameter alpha is uniform. During the relaxation process, the field reconnects and dissipates some magnetic energy as heat. The value of alpha at each time and the energy released during relaxation may be determined from the evolution of magnetic helicity. Two theorems concerning this method are proved: First, the invariance of the method with respect to gauge transformations of the vector potential is discussed, and it is shown that the helicity evolution equation in any gauge predicts the same evolution of the field. Second, it is shown that the energy release always vanishes in the limit of infinitely fast reconnection. It is found that similar footpoint motions heat an arcade more efficiently if it is already strongly sheared, such as in a rapidly evolving active region. The general conclusion is that tearing turbulence is a viable heating mechanism for the solar corona.

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