Turbulence is ubiquitous to plasmas, occurring in accretion disks, in the sun and solar wind, in the Earth's magnetosphere, and in many laboratory plasmas. In turbulence, energy cascades from very large spatial scales to very small spatial scales, eventually damping away at the dissipation scale. Many of these plasmas, however, are nearly collisionless, and therefore the mechanism by which this cascading turbulent energy is damped is not understood. In this talk I will describe initial efforts to understand the nature of magnetic reconnection in a turbulent system. We study two dimensional resistive MHD turbulence, and diagnosis the properties of the thousands of x-lines present. Implications for turbulence as well as key outstanding questions will be discussed.
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