Abstract
Reconnection is a major commonality of solar and magnetospheric physics. It was conjectured by Giovanelli in 1946 to explain particle acceleration in solar flares near magnetic neutral points. Since than it has been broadly applied in space physics including magnetospheric physics. In a special way this is due to Harry Petschek, who in 1994 published his ground breaking solution for a 2D magnetized plasma flow in regions containing singularities of vanishing magnetic field. Petschek’s reconnection theory was questioned in endless disputes and arguments, but his work stimulated the further investigation of this phenomenon like no other. However, there are questions left open. We consider two of them — “anomalous” resistivity in collisionless space plasma and the nature of reconnection in three dimensions. The Cluster and SOHO missions address these two aspects of reconnection in a complementary way — the resistivity problem in situ in the magnetosphere and the 3D aspect by remote sensing of the Sun. We demonstrate that the search for answers to both questions leads beyond the applicability of analytical theories and that appropriate numerical approaches are necessary to investigate the essentially nonlinear and nonlocal processes involved. Necessary are both micro-physical, kinetic Vlasov-equation based methods of investigation as well as large scale (MHD) simulations to obtain the geometry and topology of the acting fields and flows.
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Büchner, J. (2006). Theory and Simulation of Reconnection. In: Baker, D.N., Klecker, B., Schwartz, S.J., Schwenn, R., Von Steiger, R. (eds) Solar Dynamics and Its Effects on the Heliosphere and Earth. Space Sciences Series of ISSI, vol 22. Springer, New York, NY. https://doi.org/10.1007/978-0-387-69532-7_24
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DOI: https://doi.org/10.1007/978-0-387-69532-7_24
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