  We present estimates of the turbulent energy cascade rate, derived from a
Hall-MHD third-order law. We compute the contribution from the Hall term and
the MHD term to the energy flux. We use MMS data accumulated in the
magnetosheath and the solar wind, and compare the results with previously
established simulation results. We find that in observation, the MHD
contribution is dominant at inertial scales, as in the simulations, but the
Hall term becomes significant in observations at larger scales than in the
simulations. Possible reasons are offered for this unanticipated result.
