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PUI Acceleration at an Oblique Heliospheric Termination Shock: 2D Hybrid Kinetic Simulation

  • Authors: Masaru Nakanotani, Gary P. Zank, Marc Kornbleuth, Merav Opher

Masaru Nakanotani et al 2026 The Astrophysical Journal Letters 1001 .

  • Provider: AAS Journals

Caption: Figure 1.

Snapshots at ΩciT = 500 showing the phase-space density of the solar wind and PUI components in the top two panels, the magnetic field fluctuations, δB, in the next three panels, and the averaged magnitude of the magnetic field, ∣B∣, in the last panel. The arrow corresponds to the direction of the background magnetic field, B0. The magnetic fluctuations are normalized by B0.

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