The Role of Helicity in Magnetic Reconnection: 3D Numerical Simulations

Details The Role of Helicity in Magnetic Reconnection: 3D Numerical Simulations The Role of Helicity in Magnetic Reconnection: 3D Numerical Simulations

1999-01-05

arxiv.org/abs/astro-ph/9901039v1

Astronomy and Astrophysics

Astrophysics

AGU LaTeX manuscript, 17 pages, 2 b-w figures, 4 color plates

Scientific paper

We demonstrate that conservation of global helicity plays only a minor role in determining the nature and consequences of magnetic reconnection in the solar atmosphere. First, we show that observations of the solar coronal magnetic field are in direct conflict with Taylor's theory. Next, we present results from three-dimensional MHD simulations of the shearing of bipolar and multi-polar coronal magnetic fields by photospheric footpoint motions, and discuss the implications of these results for Taylor's theory and for models of solar activity. The key conclusion of this work is that significant magnetic reconnection occurs only at very specific locations and, hence, the Sun's magnetic field cannot relax completely down to the minimum energy state predicted by conservation of global helicity.

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