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. 2018 Aug 15;123(8):6360–6382. doi: 10.1029/2018JA025556

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©2018. The Authors.

This is an open access article under the terms of the http://creativecommons.org/licenses/by-nc-nd/4.0/ License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non‐commercial and no modifications or adaptations are made.

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(a) Model results for a source population of 0.1‐ to 10‐keV H⁺ and a flow velocity in the region beyond 10 R _E of 200 km/s; (b) model results for (the same) source population of 0.1‐ to 10‐keV H⁺ but for a flow velocity in the region beyond 10 R _E of 500 km/s; (c) model results for a source population of 0.1‐ to 10‐keV He⁺⁺, flow velocity in the region beyond 10 R _E of 500 km/s; (d) model results for a source population of 0.3‐ to 30‐keV O⁶⁺, flow velocity in the region beyond 10 R _E of 500 km/s. Note that for an observer at the dusk side of the channel (bottom of plot) at 6 R _E and V = 500 km/s, the peak energy for H⁺ is ~270 keV, the peak energy for He⁺⁺ is ~540 keV, and the peak energy for O⁶⁺ is ~1.6 MeV.