The topology of force-free magnetic fields and its implications for coronal activity

Details The topology of force-free magnetic fields and its implications for coronal activity The topology of force-free magnetic fields and its implications for coronal activity

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...312..886a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 312, Jan. 15, 1987, p. 886-894. NASA-supported research.

Mathematics

Logic

66

Force-Free Magnetic Fields, Magnetic Field Configurations, Magnetohydrodynamic Turbulence, Solar Activity, Solar Corona, Boundary Conditions, Boundary Value Problems, Photosphere, Topology

Scientific paper

The topological constraints on coronal magnetic fields are considered. For a field that is initially well-behaved and undergoes deformation by well-behaved ideal MHD motions, it is shown that the topology of the field lines in the corona can be determined at all times solely from the footpoint positions on the photospheric boundary. This result implies that the topology and, consequently, the history of the footpoint motions impose no further constraints on the field beyond those already included in the connectivity boundary conditions, so that there is no reason to expect a lack of equilibrium for fields that are initially well-behaved and evolve by ideal MHD. On the other hand, nonideal processes such as reconnection are bound to occur in the solar corona, and these may lead to magnetic topologies that have no well-bahaved Euler potentials. Hence Parker's hypothesis that footpoint motions lead to the formation of current sheets is still likely to be correct, but only if nonideal processes are included. The effects of reconnection on magnetic topology and the implications for coronal activity are discussed.

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