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Context. Three-dimensional (3D) reconnection is an important mechanism forefficiently releasing energy during astrophysical eruptive events, which isdifficult to be quantitatively analyzed especially within turbulent plasmas.  Aims. In this paper, an efficient method for identifying locations andconfigurations of 3D reconnection from MHD data is developed.  Methods. This method analyzes the local nonideal electric field and magneticstructure at an arbitrary position. As only performing algebraicalmanipulations on the discrete field data and avoiding computationally expensiveoperations like field-line tracing and root-finding, this method naturallypossesses high efficiency. To validate this method, we apply it to the 3D datafrom a high-resolution simulation of a Harris-sheet reconnection and adata-driven simulation of a coronal flux rope eruption.  Results. It is shown that this method can precisely identify the localstructures of discrete magnetic field. Through the information of nonidealelectric field and the geometric attributes of magnetic field, the localstructures of reconnection sites can be effectively and comprehensivelydetermined. For fine turbulent processes, both qualitative pictures andquantitative statistical properties of small-scale reconnection structures canbe obtained. For large-scale solar simulations, macro-scale magnetic structuressuch as flux ropes and eruption current sheets can also be recognized.  Conclusions. We develop a powerful method to analyze multi-scale structuresof 3D reconnection. It can be applied not only in MHD simulations but also inkinetic simulations, plasma experiments, and in-situ observations.

A Method for Determining the Locations and Configurations of Magnetic Reconnection within 3D Turbulent Plasmas