Is Guide Field Reconnection Inherently Turbulent?

Details Is Guide Field Reconnection Inherently Turbulent? Is Guide Field Reconnection Inherently Turbulent?

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm41d..05d&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM41D-05

Physics

[2723] Magnetospheric Physics / Magnetic Reconnection

Scientific paper

At the Earth’s magnetopause, magnetic reconnection is thought to develop within ion-scale current sheets in the presence of a finite guide field. As the dynamics develops, 2D kinetic simulations have demonstrated that new electron-scale current layers are formed extending outwards from the diffusion region, and these are often unstable to the formation of secondary islands. In this work, we demonstrate there are some profound differences in extending these previous 2D results to real 3D systems. With a finite guide field, tearing modes are unstable at resonant surfaces across the initial layer, corresponding to oblique angles relative to the standard 2D geometry. The 2D models artificially suppress these oblique modes and greatly restrict the manner in which magnetic islands can interact. In real 3D systems, both primary and secondary islands correspond to extended flux ropes, which can interact in a variety of complex ways not possible in 2D. Here, we address these challenges using Vlasov theory and 3D kinetic simulations. The theoretical results are used to gain insight into the range of unstable oblique modes and to guide and interpret 3D petascale kinetic simulations. These unprecedented simulations, using up to ~1.3 trillion particles, have revealed an inherently 3D evolution featuring the formation and interaction of flux ropes within the initial current layer, followed by the subsequent generation of secondary flux ropes within the elongated current sheets extending outward from the diffusion region as well as along the separatrices. These results may have far-reaching implications for a range of basic issues, including the structure of the exhaust, the dissipation rate of magnetic energy, the generation of stochastic magnetic fields and the transport of particles. Implications for MMS and the detections of reconnection at the dayside magnetopause are discussed

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