Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9110m&link_type=abstract
American Astronomical Society Meeting 210, #91.10; Bulletin of the American Astronomical Society, Vol. 39, p.205
Astronomy and Astrophysics
Astronomy
Scientific paper
Magnetic helicity has proven to be a powerful tool for understanding energetics of the solar corona. As it is usually defined, relative helicity is an integral over the entire coronal volume. In this work we consider two different generalizations by which relative helicity of a portion of the entire coronal volume may be calculated. Such a quantity is generally called the self helicity of the sub-volume. Each definition is a natural application of the traditional helicity formula but relative to different fields. One of the generalizations, which we term "additive self-helicity", has particularly desirable properties, such as being identically zero for any portion of a potential magnetic field. During a flare it is believed that the total helicity of the volume is conserved, but as reconnection transfers flux between domains, this will change the self-helicity of those. We demonstrate how "additive self-helicity" may be evaluated in practice to find the self-helicities for flux systems, or domains, composed of all field lines connecting a designated pair of photospheric source regions. It is then possible to quantify the transfer of self-helicity which would occur when reconnection transfers flux between flux systems.
Longcope Dana
Malanushenko Anna
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