Simulated solar wind plasma interaction with the Martian exosphere:  influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary

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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“…In many ways, such models are in good agreement with spacecraft observations (e.g. Kallio et al 2006;Modolo et al 2006;Dubinin et al 2008).…”

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

confidence: 48%

Modeling of Venus, Mars, and Titan

et al. 2011

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“…In the first we use a three-dimensional (3D) and multispecies hybrid model to provide a full description of the SW interaction with the Martian neutral environment. This simulation model has been designed by Modolo et al (2005Modolo et al ( , 2006; the hybrid kernel of the simulation program makes use of the Current Advance Method and Cyclic Leapfrog scheme (CAM-CL) designed by Matthews (1994). We resolve the Maxwell equations and self-consistently obtain a quasi-stationary solution to the global electromagnetic (EM) field as well as a description of the plasma dynamic in the vicinity of the planet.…”

Section: Simulation Modelmentioning

confidence: 99%

“…The hybrid model has been extensively described in Modolo et al (2005Modolo et al ( , 2006 and Kallio et al (2011). Solar and planetary ions are represented by sets of macroparticles, describing the full dynamics of each ion species, while electrons are described by a massless fluid that ensures the conservation of the charge neutrality of the plasma and contributes to the electronic pressure and the electric currents.…”

Section: The Hybrid Modelmentioning

confidence: 99%

Solar wind charge exchange X-ray emission from Mars

Koutroumpa¹,

Modolo²,

Chanteur³

et al. 2012

A&A

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Aims. We study the soft X-ray emission induced by charge exchange (CX) collisions between solar-wind, highly charged ions and neutral atoms of the Martian exosphere. Methods. A 3D multispecies hybrid simulation model with improved spatial resolution (130 km) is used to describe the interaction between the solar wind and the Martian neutrals. We calculated velocity and density distributions of the solar wind plasma in the Martian environment with realistic planetary ions description, using spherically symmetric exospheric H and O profiles. Following that, a 3D test-particle model was developed to compute the X-ray emission produced by CX collisions between neutrals and solar wind minor ions. The model results are compared to XMM-Newton observations of Mars. Results. We calculate projected X-ray emission maps for the XMM-Newton observing conditions and demonstrate how the X-ray emission reflects the Martian electromagnetic structure in accordance with the observed X-ray images. Our maps confirm that X-ray images are a powerful tool for the study of solar wind-planetary interfaces. However, the simulation results reveal several quantitative discrepancies compared to the observations. Typical solar wind and neutral coronae conditions corresponding to the 2003 observation period of Mars cannot reproduce the high luminosity or the corresponding very extended halo observed with XMM-Newton. Potential explanations of these discrepancies are discussed.

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“…In Modolo et al [2005], planetary ions are produced through ionisation of the exosphere either by solar photons, electronic impacts or charge exchanges. Details concerning the chosen neutral environment, as well as the implementation of the ionization mechanisms, are given in Modolo et al [2005Modolo et al [ , 2006. As shown by Modolo et al [2006] both the position and the shape of the Martian BS are weakly sensitive to the solar activity, hence the conditions of solar maximum used in the hybrid simulation are not expected to play a major role in the present study.…”

Section: Hybrid Simulationmentioning

confidence: 99%

“…Details concerning the chosen neutral environment, as well as the implementation of the ionization mechanisms, are given in Modolo et al [2005Modolo et al [ , 2006. As shown by Modolo et al [2006] both the position and the shape of the Martian BS are weakly sensitive to the solar activity, hence the conditions of solar maximum used in the hybrid simulation are not expected to play a major role in the present study. Mazelle et al [2004] have discussed the structure of the Martian BS: its thickness is comparable to the convective gyroradius of SW protons in the quasi-perpendicular region, except in the vicinity of the subsolar point where it is smaller.…”

Section: Hybrid Simulationmentioning

confidence: 99%

Reflection of solar wind protons on the Martian bow shock: Investigations by means of 3‐dimensional simulations

Richer¹,

Chanteur²,

Modolo³

et al. 2012

Geophysical Research Letters

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[1] The reflection of solar wind protons on the Martian bow shock (BS) is investigated by means of three-dimensional simulation models. A two steps approach is adopted to allow a detailed analysis of the reflected population. Firstly, the 3-dimensional hybrid model of Modolo et al. (2005) is used to compute a stationary state of the interaction of the solar wind (SW) with Mars. Secondly, the motion of test particles is followed in the electromagnetic field computed by the hybrid simulation meanwhile detection criteria defined to identify reflected protons are applied. This study demonstrates some effects of the large curvature of a planetary BS on the structure of the foreshock. Reflected protons encounter the BS in a region encompassing parts of the quasi-perpendicular and quasi-parallel shocks, and exit the shock mainly from the quasi-parallel region. The energy spectrum of all reflected protons extends from 0 to almost 15keV. A virtual omnidirectional detector (VOD) is used to compute the local omnidirectional flux of reflected protons at various locations upstream of the BS. Spatial variations of this omnidirectional flux indicate the location and spatial extent of the proton foreshock and demonstrate its shift, increasing with the distance downstream, in the direction opposite to the motional electric field of the SW. Local energy spectra computed from the VOD observations demonstrate the existence of an energy gradient along the direction of the convection electric field.Citation: Richer, E., G. M. Chanteur, R. Modolo, and E. Dubinin (2012), Reflection of solar wind protons on the Martian bow shock: Investigations by means of 3-dimensional simulations, Geophys.

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Simulated solar wind plasma interaction with the Martian exosphere: influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary

Cited by 59 publications

References 45 publications

Modeling of Venus, Mars, and Titan

Modeling of Venus, Mars, and Titan

Solar wind charge exchange X-ray emission from Mars

Reflection of solar wind protons on the Martian bow shock: Investigations by means of 3‐dimensional simulations

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