http://arxiv.org/abs/1904.11173
Solving the problem of fast eruptive events in magnetically dominated astrophysical plasmas requires the use of particularly well adapted numerical tools. Indeed, the central mechanism based on magnetic reconnection is determined by a complex behavior with quasi-singular forming current layers enriched by their associated small scale magnetic islands called plasmoids. A new code for the solution of two dimensional dissipative magnetohydrodynamics (MHD) equations in cartesian geometry specifically developed to this end is thus presented. A current-vorticity formulation representative of an incompressible model is chosen in order to follow the formation of the current sheets and the ensuing magnetic reconnection process. A finite element discretization using triangles with quadratic basis functions on an unstructured grid is employed, and implemented via a highly adaptive characteristic- Galerkin scheme. The adaptivity of the code is illustrated on simplified test equations and finally for magnetic reconnection associated to the non linear development of the tilt instability between two repelling current channels. Varying the Lundquist number S, has allowed to study the transition between the steady-state Sweet-Parker reconnection regime (for S < 10^4) and plasmoids dominated reconnection one (for S > 10^5). The implications for the understanding of the mechanism explaining the fast conversion of free magnetic energy in astrophysical environments such as in solar corona are briefly discussed.
H. Baty
Fri, 26 Apr 19
67/69
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