Background and pickup ion velocity distribution dynamics in Titan’s plasma environment: 3D hybrid simulation and comparison with CAPS T9 observations
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Date
2011-05-30
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Citation of Original Publication
Lipatov, A. S., E. C. Sittler, R. E. Hartle, J. F. Cooper, and D. G. Simpson. “Background and Pickup Ion Velocity Distribution Dynamics in Titan’s Plasma Environment: 3D Hybrid Simulation and Comparison with CAPS T9 Observations.” Advances in Space Research 48, no. 6 (September 15, 2011): 1114–25. https://doi.org/10.1016/j.asr.2011.05.026.
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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Public Domain Mark 1.0
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Abstract
In this report we discuss the ion velocity distribution dynamics from the 3D hybrid simulation. In our model the background, pickup, and ionospheric ions are considered as a particles, whereas the electrons are described as a fluid. Inhomogeneous photoionization, electron-impact ionization and charge exchange are included in our model. We also take into account the collisions between the ions and neutrals. The current simulation shows that mass loading by pickup ions H⁺, H⁺₂, CH₄ and N⁺₂ is stronger than in the previous simulations when O⁺ ions are introduced into the background plasma. In our hybrid simulations we use Chamberlain profiles for the atmospheric components. We also include a simple ionosphere model with average mass M = 28 amu ions that were generated inside the ionosphere. The moon is considered as a weakly conducting body. Special attention will be paid to comparing the simulated pickup ion velocity distribution with CAPS T9 observations. Our simulation shows an asymmetry of the ion density distribution and the magnetic field, including the formation of the Alfvén wing-like structures. The simulation also shows that the ring-like velocity distribution for pickup ions relaxes to a Maxwellian core and a shell-like halo.