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Fig. 3. | Earth, Planets and Space

Fig. 3.

From: Magnetic shadowing of high energy ions at Mars and how this effect can be simulated using a hybrid model

Fig. 3.

The motion of solar wind Hsw+ ions which have the solar wind bulk velocity in four upstream cases: (a) the nominal run where Usw = 485 km s–1, nsw = 2.7 cm−3, IMF = [−1.634, 2.516, 0] nT, (b) the high velocity 2 × Usw run where Usw = 970 km s−1, nsw = 2.7 cm−3, IMF = [−1.634, 2.516, 0] nT, (c) the high density 4 × nsw run where Usw = 485 km s−1, nsw = 10.8 cm−3, IMF = [−1.634, 2.516, 0] nT and (d) the high density and high IMF 4 × nsw2 × IMF run where Usw = 485 km s−1, nsw = 10.8 cm−3, IMF = [−6.536, 10064, 0] nT. The initial temperature of the test particles was zero and they were generated near the x = 10,000 km plane on the 15 (y -direction) × 15 (z-direction) grid. The color in the y = 0 noon-midnight meridian planes shows the total density of protons. The white lines show test particle orbits. The horizontal and the vertical lengths are each from −10,000 km to 10,000 km. Note the presence of the low density Hsw+ “solar wind-flow shadow” behind the planet (dark blue areas).

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