Formation of Alfvén wave ducts by magnetotail flow bursts

Observations show that among its various magnetospheric sources, Alfvenic Poynting flux from the magnetotail reaches the ionosphere with the greatest intensity. Dayside fluxes are statistically weaker though more persistent.

Flankside fluxes are weakest. We show using global magnetohydrodynamic simulations that these distributions can be attributed to the formation (or not) of meridionally narrow, relatively uniform, low Alfven conductance channels that efficiently transmit Alfvenic power to the near-Earth space. These Alfven ducts form naturally at the heads of flow bursts in the magnetotail but not in flankside flux tubes, where the transmission of Alfvenic power is strongly attenuated by reflections at large conductance gradients along the propagation path.