Yi-Min Huang, Goddard Space Flight Center  Magnetic Chaos, Reconnection, and Dissipation: A New Look at Coronal Heating  The constant shuffling of coronal loop footpoints by photospheric convection entangles the Sun's magnetic field, leading to a complex topology. In Parker's influential coronal heating model, this entanglement produces a large number of small-scale magnetic reconnection events, or "nanoflares," which are thought to heat the corona to millions of degrees. This work uses Parker's model as a testbed to investigate whether chaotic magnetic fields-a generic feature of such 3D systems-naturally facilitate fast reconnection by exploiting the sensitivity of field line mapping to non-ideal effects. Furthermore, we present an extension of these simulations that incorporates two-fluid physics to explore if the overall energy dissipation is sensitive to the detailed microphysics of the reconnection process. Our results shed new light on the fundamental link between large-scale external forcing and small-scale energy release in the solar corona.