Modeling of Venus, Mars, and Titan

Kallio, Esa; Chaufray, Jean‐Yves; Modolo, Ronan; Snowden, D.; Winglee, R. M.

doi:10.1007/978-1-4614-3290-6_8

Cited by 14 publications

(13 citation statements)

References 151 publications

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“…This approach, although more binding in terms of computational resources than a fluid model, is based on less assumption and include more physics (Hall term, Larmor radius effect, etc.). A complete review of these formalisms, their respective assumptions and limitations are detailed in Ledvina et al [], Kallio et al [], and Winske et al [].…”

Section: Simulation Modelmentioning

confidence: 99%

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

et al. 2016

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In order to better represent Mars‐solar wind interaction, we present an unprecedented model achieving spatial resolution down to 50 km, a so far unexplored resolution for global kinetic models of the Martian ionized environment. Such resolution approaches the ionospheric plasma scale height. In practice, the model is derived from a first version described in Modolo et al. (2005). An important effort of parallelization has been conducted and is presented here. A better description of the ionosphere was also implemented including ionospheric chemistry, electrical conductivities, and a drag force modeling the ion‐neutral collisions in the ionosphere. This new version of the code, named LatHyS (Latmos Hybrid Simulation), is here used to characterize the impact of various spatial resolutions on simulation results. In addition, and following a global model challenge effort, we present the results of simulation run for three cases which allow addressing the effect of the suprathermal corona and of the solar EUV activity on the magnetospheric plasma boundaries and on the global escape. Simulation results showed that global patterns are relatively similar for the different spatial resolution runs, but finest grid runs provide a better representation of the ionosphere and display more details of the planetary plasma dynamic. Simulation results suggest that a significant fraction of escaping O+ ions is originated from below 1200 km altitude.

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Section: Simulation Modelmentioning

confidence: 99%

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

et al. 2016

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“…In addition to the theoretic analysis, numerical simulations (e.g., MHD simulations and hybrid simulations) performed to study the induced magnetosphere may help to provide hints to understand the tail configuration, although derived simulation results must be interpreted with caution [ Kallio et al ., ]. Hybrid simulations of Titan [ Simon and Motschmann , ] and Venus [ Kallio et al ., ] showed that the current sheet of the induced magnetotail would be displaced when there is a corresponding IMF flow‐aligned component.…”

Section: Discussionmentioning

confidence: 99%

Is the flow‐aligned component of IMF really able to impact the magnetic field structure of Venusian magnetotail?

et al. 2016

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An earlier statistical survey suggested that the flow‐aligned component of upstream interplanetary magnetic field (IMF) may play an important role in controlling the lobe asymmetries of the Venusian magnetotail. The tail current sheet would be displaced and the magnetic field configuration would show asymmetries with respect to the current sheet. The asymmetries are expected to be more evident when the flow‐aligned component becomes dominant. Here with carefully selected cases as well as a statistical study based on Venus Express observations in the near‐Venus tail, we show that the lobe asymmetries of the magnetic field as well as the displacement of the current sheet are common characteristics of the Venusian magnetotail. However, the asymmetries and the displacement of the current sheet do not show a significant dependence on the flow‐aligned component of the IMF. Our results suggest that the flow‐aligned component of IMF cannot penetrate into the near magnetotail to impact the magnetic field structure.

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“…The CEM can be biased at different potentials ranging from 1000 to 2500 V. The gain of the CEM is a function of both the bias voltage and the ion mass; the typical gain for CEM is ~10 5 . Partial pressures of ~10 -14 torr can be measured with the CEM.…”

Section: Instrumentmentioning

confidence: 99%

“…The Martian exosphere starts from an altitude of ~250 km (ref. 5). The only inferences drawn on the Martian exosphere, so far, have been on its total number density based on spacecraft drag measurements and few studies on the extent of hydrogen 6 and oxygen exospheres 7 based on their respective spectral emission signatures.…”

Section: Introductionmentioning

confidence: 99%

“…The observation of Mars exospheric X-rays using the Reflection Grating Spectrometer/XMM Newton suggests the presence of a neutral exosphere up to ~8 Martian radii 2 . In addition, there have been extensive modelling studies to predict the composition and distribution of the Martian neutral exosphere 5,[10][11][12][13] . All these studies indicate that there exists a neutral exosphere around Mars that extends several thousands of kilometres.…”

Section: Introductionmentioning

confidence: 99%

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