Three-dimensional hybrid simulation of magnetized plasma flow around an obstacle

Shimazu, H.

doi:10.1186/bf03352242

Cited by 27 publications

(33 citation statements)

References 22 publications

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“…Plate lb shows that a magnetic barrier, where the magnetic field is larger than the typical value elsewhere, formed around the planet. These results are the same as those of Shimazu [1999] Plate 3c shows that the planetary oxygen ions escape into the solar wind on the lower side. They can escape from the planet and be picked up by the solar wind because their Larmor radius is larger than the width of the magnetic barrier.…”

Section: ] (5 X 1025supporting

confidence: 78%

“…The other difference between the present simulation code and that of Shimazu [1999] is that there are twice as many grid cells in each direction. In the previous study of Shimazu [1999], fine structure in the shock could not be observed because of the sparse grid cells used.…”

Section: Modelmentioning

confidence: 99%

“…The simulation code used here is the same as that used by Shimazu [1999], but with two differences. One is that the planet is treated as an ionized gaseous body in this model.…”

Section: Modelmentioning

confidence: 99%

“…One is that the planet is treated as an ionized gaseous body in this model. Shimazu [1999] treated the planet as a solid sphere whose surface absorbed or reflected particles. This assumption made it difficult to consider realistic ion behavior near the planet.…”

Section: Modelmentioning

confidence: 99%

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Three‐dimensional hybrid simulation of solar wind interaction with unmagnetized planets

Shimazu¹

2001

J. Geophys. Res.

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Abstract. The interaction between the solar wind and unmagnetized planets was investigated using computer simulation and a three-dimensional hybrid code that treats kinetic ions and massless fluid electrons. In the simulation the planet was treated as an ionized gaseous body with uniform and constant supply of plasma. The results given in this paper showed that the shock size and magnetic barrier intensity are asymmetrical in the direction of the convection electric field because of oxygen ions escaping from the side of the planet to which the electric field was pointing. The calculated asymmetry in the magnetic barrier intensity was consistent with observations, although the direction of the calculated asymmetry in the shock size did not match the asymmetry observed near either Venus or Mars. When the planet size was comparable to the Larmor radius of protons, a multiple-shock structure was observed in the simulation. It is suggested that this structure is due to dispersion of the magnetosonic waves caused by the finite Larmor radius of protons. The simulation results also showed that ions escaped to the magnetotail through the tail rays and that the tail rays were connected with the plasma sheet. In the previous hybrid simulation studies, the planet was treated as a solid sphere whose surface absorbed or reflected 8333

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Section: ] (5 X 1025supporting

confidence: 78%

Section: Modelmentioning

confidence: 99%

“…The simulation code used here is the same as that used by Shimazu [1999], but with two differences. One is that the planet is treated as an ionized gaseous body in this model.…”

Section: Modelmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

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Three‐dimensional hybrid simulation of solar wind interaction with unmagnetized planets

Shimazu¹

2001

J. Geophys. Res.

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“…Various hybrid simulation studies have been made of the solar-wind-ionosphere interaction of unmagnetized planets (Modolo et al, 2006(Modolo et al, , 2005Bößwetter et al, 2004;Janhunen, 2002, 2001;Shimazu, 2001Shimazu, , 1999Brecht, 1997;Brecht et al, 1993). The hybrid simulations treat ions as particles while electrons are considered as a massless charge-neutralizing fluid.…”

Section: Published By Copernicus Publications On Behalf Of the Europementioning

confidence: 99%

IMF-induced escape of molecular ions from the Martian ionosphere

et al. 2013

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Since Mars does not possess a significant global intrinsic magnetic field, the solar wind interacts directly with the Martian ionosphere and can induce ion escapes from it. Phobos-2 and recent Mars Express (MEX) observations have shown that the escaping ions are O⁺ as well as molecular O₂⁺ and CO₂⁺. While O⁺ escape can be understood by the ion pick-up of non-thermal O corona extended around the planet, regarding the heavy molecular O₂⁺ and CO₂⁺, which are buried in the lower ionosphere, a novel escape mechanism needs to considered. Here we attack this problem by global magnetohydrodynamic (MHD) simulations. First, we clarify the global structure of the streamlines that result from the interaction with the solar wind. Then, by focusing on the streamlines that dip into the low-altitude part of the dayside ionosphere, we investigate the escape path of the molecular ions. The effects of the interplanetary magnetic field (IMF) on the molecular ion escape process are investigated by comparing the results with and without IMF. IMF has little effect on O⁺ escape via ion pick-up mediated by solar wind electron impact ionization of the O corona. O₂⁺ and CO₂⁺ are shoveled from the low-altitude regions of the dayside ionosphere by magnetic tension in the presence of IMF. These ions are pulled by the U-shaped field lines to the north and south poles, and at the terminator, they are concentrated in the noon–midnight meridian plane. These ions remain confined to the noon–midnight plane as they are transported to the nightside to form the tail ray. Then they escape along the streamlines open to the interplanetary space. Under a typical solar wind and IMF condition expected at Mars, O⁺, O₂⁺ and CO₂⁺ escape fluxes are 8.0 × 10²³, 3.5 × 10²³ and 5.0 × 10²² ion s⁻¹, respectively, which are in good agreement with the MEX observations

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Oxygen Ion Energization at Mars: Comparison of MAVEN and Mars Express Observations to Global Hybrid Simulation

et al. 2018

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We study oxygen ion energization in the Mars‐solar wind interaction by comparing particle and magnetic field observations on the Mars Atmosphere and Volatile EvolutioN (MAVEN) and Mars Express missions to a global hybrid simulation. We find that large‐scale structures of the Martian‐induced magnetosphere and plasma environment as well as the Mars heavy ion plume as seen by multispacecraft observations are reproduced by the model. Using the simulation, we estimate the dynamics of escaping oxygen ions by analyzing their distance and time of flight as a function of the gained kinetic energy along spacecraft trajectories. In the upstream region the heavy ion energization resembles single‐particle solar wind ion pickup acceleration as expected, while within the induced magnetosphere the energization displays other features including the heavy ion plume from the ionosphere. Oxygen ions take up to 80 s and travel the distance of 20,000 km after their emission from the ionosphere to the induced magnetosphere or photoionization from the neutral exosphere before they have reached energies of 10 keV in the plume along the analyzed spacecraft orbits. Lower oxygen ion energies of 100 eV are reached faster in 10–20 s over the distance of 100–200 km in the plume. Our finding suggests that oxygen ions are typically observed within the first half of their gyrophase if the spacecraft periapsis is on the hemisphere where the solar wind convection electric field points away from Mars.

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Three-dimensional hybrid simulation of magnetized plasma flow around an obstacle

Cited by 27 publications

References 22 publications

Three‐dimensional hybrid simulation of solar wind interaction with unmagnetized planets

Three‐dimensional hybrid simulation of solar wind interaction with unmagnetized planets

IMF-induced escape of molecular ions from the Martian ionosphere

Oxygen Ion Energization at Mars: Comparison of MAVEN and Mars Express Observations to Global Hybrid Simulation

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