Modeling and Simulating Flowing Plasmas and Related Phenomena

Ledvina, S. A.; Ma, Y.; Kallio, Esa

doi:10.1007/s11214-008-9384-6

Cited by 99 publications

(89 citation statements)

References 120 publications

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“…Interested readers can find descriptions of the Vlasov model and its usage in planetary atmospheres/ionospheres (e.g. Schunk and Nagy 2009) as well as recent reviews of MHD and hybrid modeling approaches (Ma et al 2008;Ledvina et al 2008) from the literature.…”

Section: Self-consistent Plasma Modeling Methodsmentioning

confidence: 99%

“…In this section we briefly review the methods of several fluid models. Ledvina et al (2008) is a more comprehensive review of MHD modeling methods, assumptions, and limitations. We start with ideal MHD, which is the basis for all MHD models but is rarely used to study the plasma interactions of VMT today.…”

Section: Magnetohydrodynamic Methodsmentioning

confidence: 99%

“…In Table 1, the implicit length scales of various MHD assumptions are compared to a typical scale size of simulations at VMT, L ∼ 0.1R. The scale sizes in Table 1 are taken from Ledvina et al (2008) and are calculated for values applicable to the solar wind (for Mars and Venus) and for magnetospheric O + for Titan. The term in the first row of the table, r l /L, compares the Lamour radius of ions in the induced magnetosphere to the simulation scale length.…”

Section: Assumptions Of Mhd Modelsmentioning

confidence: 99%

“…Some MHD equations such as the multifluid equations cannot be conservative. The errors resulting from using non-conservative forms of MHD equations are not well understood and we refer the reader to Ledvina et al (2008) for a more detailed description of this issue.…”

Section: Ideal Mhdmentioning

confidence: 99%

“…The multi-fluid method used by Najib et al (2011) includes source and loss terms as well as ion-neutral and ion-ion collision terms in the continuity, mass, and pressure equations. As described in Ledvina et al (2008), there are questions related to how multi-fluid models simulate shocks. When one species shocks in a hybrid simulation waves are produced that interact with other ion particles.…”

Section: Multi-fluidmentioning

confidence: 99%

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Modeling of Venus, Mars, and Titan

et al. 2011

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Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn's moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects.

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Section: Self-consistent Plasma Modeling Methodsmentioning

confidence: 99%

Section: Magnetohydrodynamic Methodsmentioning

confidence: 99%

Section: Assumptions Of Mhd Modelsmentioning

confidence: 99%

Section: Ideal Mhdmentioning

confidence: 99%

Section: Multi-fluidmentioning

confidence: 99%

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Modeling of Venus, Mars, and Titan

et al. 2011

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Electrodynamics of the Martian dynamo region near magnetic cusps and loops

Riousset

Paty

Lillis

et al. 2014

Geophysical Research Letters

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Strong and inhomogeneous remanent magnetization on Mars results in a complex pattern of crustal magnetic fields. The geometry and topology of these fields lead to atmospheric electrodynamic structures that are unique among the bodies of the solar system. In the atmospheric dynamo region (∼100−250 km altitude), ions depart from the gyropath due to collisions with neutral particles, while electron motion remains governed by electromagnetic drift. This differential motion of the charge carriers generates electric currents, which induce a perturbation field. The electromagnetic changes ultimately alter the behavior of the local ionosphere beyond the dynamo region. Here we use multifluid modeling to investigate the dynamics around an isolated magnetic cusp and around magnetic loops or arcades representative of the magnetic topology near, for example, Terra Sirenum. Our results show consistent, circular patterns in the electric current around regions with high local field strength, with possible consequences on atmospheric escape of charged particles.

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Energization of planetary pickup ions in the solar system

Järvinen

Kallio

2014

JGR Planets

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We study the solar wind-induced ion escape from planetary atmospheres at different radial heliospheric distances in the solar system. We derive histograms of the gyroaveraged E × B velocities, energies, and Larmor radii of planetary ions in the solar wind at Mercury, Venus, Earth, and Mars. The statistical analysis is based on the interplanetary Pioneer Venus Orbiter and OMNI solar wind data sets. In addition to the energization in the undisturbed solar wind we also model how planetary heavy ions get energized in the solar wind interaction of an unmagnetized planet at different distances to the Sun. We found that due to the Parker spiral, pickup ions are expected to be found on average at lower energies and at velocities more perpendicular to the solar wind flow, the closer to the Sun a planet or a comet is. According to a global hybrid simulation, planetary heavy ion energization is influenced qualitatively in a similar way in the presence of an induced magnetosphere than in the upstream solar wind under different Parker spiral angles due to fact that the structure of an induced magnetosphere depends strongly on the interplanetary magnetic field and solar wind conditions. Finally, the energization and dynamics of the pickup ions vary considerably with the solar activity. The variation is stronger the farther away from the Sun an object is. The Larmor radii of the pickup ions are largest during a solar minimum while the pickup ion energies are highest during the declining phase of a solar cycle.

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Modeling and Simulating Flowing Plasmas and Related Phenomena

Cited by 99 publications

References 120 publications

Modeling of Venus, Mars, and Titan

Modeling of Venus, Mars, and Titan

Electrodynamics of the Martian dynamo region near magnetic cusps and loops

Energization of planetary pickup ions in the solar system

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