Authors: Hayden Atkinson (University of Delaware), Michael Shay (University of Delaware)

Magnetic reconnection is known to occur throughout the heliosphere, and may play an important role in dissipating turbulent fluctuations. Recent simulation and observational studies have shown that the distribution of reconnection rates are strongly with the distribution of turbulent fluctuations at the energy containing scale. While the global amount of reconnection occurring in simulations is straightforward to calculate, estimating this rate directly from satellite observations poses a unique challenge. We take the first steps in this work by examining virtual satellite passes in MHD simulations of turbulence, determining the best signatures to use to find reconnection sites, and then studying how this information can be used to estimate the prevalence of reconnection. In particular, we examine the variation quantities such as the magnitude of the magnetic field, the Hessian determinant of the magnetic potential, the electric field and the current density. Using these values, we estimate the global reconnection rate and compare it to the value calculated directly from the simulation.