Non-Coplanar Magnetic Reconnection as a Magnetic Twist Origin

Details Non-Coplanar Magnetic Reconnection as a Magnetic Twist Origin Non-Coplanar Magnetic Reconnection as a Magnetic Twist Origin

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jkas...32..137c&link_type=abstract

Journal of the Korean Astronomical Society, vol. 32, no. 2, pp. 137-147

Astronomy and Astrophysics

Astronomy

7

Mhd, Sun: Magnetic Fields

Scientific paper

Recent studies show the importance of understanding three-dimensional magnetic reconnection on the solar surface. For this purpose, I consider non-coplanar magnetic reconnection, a simple case of three-dimensional reconnection driven by a collision of two straight flux tubes which are not on the same plane initially. The relative angle theta between the two tubes characterizes such reconnection, and can be regarded as a measure of magnetic shear. The observable characteristics of non-coplanar reconnection are compared between the two cases of small and large angles. An important feature of the non-coplanar reconnection is that magnetic twist can be produced via the re-ordering of field lines. This is a consequence of the conversion of mutual helicity into self helicities by reconnection. It is shown that the principle of energy conservation when combined with the production of magnetic twist puts a low limit on the relative angle between two flux tubes for reconnection to occur. I provide several observations supporting the magnetic twist generation by reconnection, and discuss its physical implications for the origin of magnetic twist on the solar surface and the problem of coronal heating.

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