A comparison of global models for the solar wind interaction with Mars

Brain, David; Barabash, S.; Boesswetter, A.; Bougher, S. W.; Brecht, S. H.; Chanteur, Gérard; Crider, D. H.; Dubinin, E.; Fang, Xiaohua; Fräenz, M.; Halekas, J. S.; Harnett, E. M.; Holmström, Mats; Kallio, Esa; Lämmer, H.; Ledvina, S. A.; Liemohn, Michael W.; Liu, Kaijun; Luhmann, J. G.; Ma, Yingjuan; Modolo, Ronan; Nagy, A. F.; Motschmann, U.; Nilsson, Hans; Shinagawa, Hiroyuki; Simon, S.; Terada, Naoki

doi:10.1016/j.icarus.2009.06.030

Cited by 114 publications

(118 citation statements)

References 86 publications

(144 reference statements)

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“…Similar to the findings of Brain et al (2010), that were based on Mars Global Surveyor measurements, in regions where the magnetic field was oriented horizontal to the surface the penetration of solar wind protons was minimal, however where the field lines were radial to the surface the density and temperature of solar wind protons was enhanced. This effect was studied for several solar wind velocities and densities as well as magnetic field orientations and for one extreme storm-like event.…”

Section: Mhd Models Of Mars' Interaction With the Solar Windsupporting

confidence: 85%

“…Najib et al (2011) noted that the asymmetries simulated by multi-fluid models due to the individual Lorentz forcing of ion species are similar to the asymmetries observed in hybrid models. However, a comparison paper by Brain et al (2010) shows that the ion outflow predicted by hybrid, multi-fluid and MHD simulations can be quite different. Brain et al (2010) presented a comprehensive comparison of MHD, multi-fluid, and hybrid modeling techniques that have been recently used to study Mars' plasma interaction.…”

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

“…However, a comparison paper by Brain et al (2010) shows that the ion outflow predicted by hybrid, multi-fluid and MHD simulations can be quite different. Brain et al (2010) presented a comprehensive comparison of MHD, multi-fluid, and hybrid modeling techniques that have been recently used to study Mars' plasma interaction. Brain et al (2010) showed that even with identical upstream conditions and similar inner boundary conditions various MHD, multi-fluid, and hybrid models can produce noticeably different results, and that the differences from model to model are not always easy to explain.…”

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

“…Brain et al (2010) presented a comprehensive comparison of MHD, multi-fluid, and hybrid modeling techniques that have been recently used to study Mars' plasma interaction. Brain et al (2010) showed that even with identical upstream conditions and similar inner boundary conditions various MHD, multi-fluid, and hybrid models can produce noticeably different results, and that the differences from model to model are not always easy to explain. For example, in MHD models most ions escape directly downstream in the solar wake.…”

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

“…Based on these results, Brain et al (2010) questioned whether the large-scale downstream outflow of ions in fluid models was physically realistic at all. Not surprisingly, the different mechanisms of ion outflow and the differences in ionospheric configuration lead to large differences in the calculated ion escape rates.…”

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

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: Mhd Models Of Mars' Interaction With the Solar Windsupporting

confidence: 85%

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

Section: Mhd Models Of Mars' Interaction With the Solar Windmentioning

confidence: 99%

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Modeling of Venus, Mars, and Titan

et al. 2011

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Directionality and variability of energetic neutral hydrogen fluxes observed by Mars Express

et al. 2013

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[1] Using data collected by the neutral particle detector of the analyzer of space plasmas and energetic atoms on board Mars Express, we establish the global morphology of hydrogen energetic neutral atom (ENA) fluxes. The observations were conducted in March-July 2004 and reveal that low flux ENAs (< 5 10 5 cm -2 s -1 sr -1 ) are emitted roughly isotropically from the dayside of the planet. These ENA emissions originate from the backscattering of the hydrogen ENAs produced by the charge exchange of the upstream solar wind in the extended Martian exosphere. ENAs of higher fluxes are emitted preferentially in the directions perpendicular to the undisturbed solar wind velocity. This population is due to the charge exchange of the magnetosheath plasma. At a great distance, these ENA emissions resemble a thick layer or a wall. The emissions are enhanced in the direction opposite to the convective electric field (E c ). This enhancement reflects the asymmetric shape of the induced magnetic boundary that is close to the planet hemisphere where the E c points toward the Sun-Mars line (-E c hemisphere). The ENA flux shows a positive correlation with the solar wind dynamic pressure. The asymmetry in the ENA emissions is modest during quiet solar wind conditions but becomes more pronounced when the solar wind dynamic pressure increases.

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Asymmetries of the magnetic field line draping shape around Venus

Wang

Zhang

et al. 2013

JGR Space Physics

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[1] The magnetic field data observed by Venus Express (VEX) from April 2006 to December 2009 are analyzed in order to describe the magnetic configuration around Venus. All the magnetic observations are organized in a coordinate system which is determined by the solar wind (SW) flow and the interplanetary magnetic field. By averaging and compiling the VEX data, we compile a global picture of the magnetic field for the SW interaction with Venus. The magnetic field around the planet displays a clear asymmetry on both field strength and pattern. The magnetic field is stronger on the +E hemisphere where the convective electric field ! E SW points away from the planet, and is wrapped around the planet more tightly on the -E hemisphere where ! E SW points toward the planet. The underlying physics of this ! E SW asymmetry is still under debate. Except in ideal single-fluid MHD simulation, the ! E SW asymmetry can be observed in both multifluid MHD and hybrid simulations.

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A comparison of global models for the solar wind interaction with Mars

Cited by 114 publications

References 86 publications

Modeling of Venus, Mars, and Titan

Modeling of Venus, Mars, and Titan

Directionality and variability of energetic neutral hydrogen fluxes observed by Mars Express

Asymmetries of the magnetic field line draping shape around Venus

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