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Magnetic Reconnection in 3D vs. 2D and Dependency on Magnetic Shear

Presentation #102.07 in the session Coronal Heating: Present Understanding and Future Progress I.

Published onOct 20, 2022
Magnetic Reconnection in 3D vs. 2D and Dependency on Magnetic Shear

Magnetic reconnection plays a central role for heating the solar coronal plasma — including during fares — as well as other places in the heliosphere and beyond, where each event can be characterized by its geometry and magnetic configurations, forming structures that we can categorize to be more 2D or 3D. Although the difference between reconnection rates in 2D and 3D has been noted before, we perform a comprehensive study and offer a possible explanation. We report on a study of the reconnection rate using the resistive MHD code LaRe3D. We show that the rate depends strongly on the existence and interaction of different tearing layers (oblique tearing modes) within the current sheet. Such modes are only present with a finite guide feld and a spatial dependence in this third direction. We fnd, as have others, that reconnection rates are artificially high in 2D simulations, and we offer an explanation.

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