Statistics of the turbulent energy transfer rate conditioned on magnetic field line topology in the solar wind

The evolving subset of turbulent structures facilitates the energy transfer from large to small spatial scales, on average. Currently, it is not known how the discontinuities that develop between these structures alter the energy transfer in the solar wind. Quantifying the energy transfer to small scales is essential to explain the apparent plasma heating during its advection through the heliosphere. We analyse the energy transfer rate conditioned on the magnetic field line topology of the associated structures in the solar wind. Magnetic field line topology is classified using invariants of the magnetic field gradient tensor constructed from the Cluster spacecraft configuration on scale of approximately 40 proton gyro-radii. Third order structure functions are estimated for five solar wind intervals and conditioned on the contemporaneous values of the topological invariants. We determine how the global mean energy transfer rates correlate with the topology of the turbulence.