A comparison of magnetohydrodynamic instabilities at the Martian ionopause

Penz, T.; Arshukova, I. L.; Terada, Naoki; Shinagawa, Hiroyuki; Еркаев, Н. В.; Biernat, H. K.; Lämmer, H.

doi:10.1016/j.asr.2004.11.039

Cited by 15 publications

(15 citation statements)

References 18 publications

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“…Their ion loss rates of (2–30) × 10 23 s −1 are thus limited to loss of ions in detached plasma clouds, but are comparable to loss rates for ion outflow computed from MHD models. Penz et al [2005] expanded the study to other wave instabilities, such as the Rayleigh‐Taylor instability.…”

Section: Discussionmentioning

confidence: 99%

Morphology of the dayside ionosphere of Mars: Implications for ion outflows

Fox

2009

J. Geophys. Res.

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[1] Significant fluxes of tailward streaming ions have been detected in the Martian wake by instruments on spacecraft. Imposing outward fluxes at the top of a model will produce dayside ion density profiles that are characterized by smaller scale heights than those of diffusive equilibrium. We determine the maximum outward fluxes of ions, and those implied by radio occultation data, by constructing $180 models, with upward velocity boundary conditions in the range from 0 to (7-8) Â 10 5 cm s À1 in small increments. As the upward velocity is increased, the topside ion or electron densities decrease until eventually the computed ion fluxes cease to increase, implying that this is the maximum outward flux that the ionosphere can sustain. By comparison to data, we derive a low solar activity upward flux of O

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Section: Discussionmentioning

confidence: 99%

Morphology of the dayside ionosphere of Mars: Implications for ion outflows

Fox

2009

J. Geophys. Res.

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“…Details such as plasma velocity shear and density gradient size may also be a factor outside of crustal regions if the Kelvin Helmholz instability occurs near the Martian ionopause flanks as it is proposed to occur at Venus (e.g. Penz et al 2005).…”

Section: How Does the Upper Boundary Of The Ionosphere The Ionopausementioning

confidence: 97%

The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere Reservoir That Regulates Volatile Escape

et al. 2014

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The Mars thermosphere-ionosphere-exosphere (TIE) system constitutes the atmospheric reservoir (i.e. available cold and hot planetary neutral and thermal ion species) that regulates present day escape processes from the planet. The characterization of this TIE system, including its spatial and temporal (e.g., solar cycle, seasonal, diurnal, episodic) variability is needed to determine present day escape rates. Without knowledge of the physics and chemistry creating this TIE region and driving its variations, it is not possible to constrain either the short term or long term histories of atmosphere escape from Mars. MAVEN (Mars Atmosphere and Volatile Evolution Mission) will make both in-situ and remote measurements of the state variables of the Martian TIE system. A full characterization of the thermosphere (∼100-250 km) and ionosphere (∼100-400 km) structure (and its variability) will be conducted with the collection of spacecraft in-situ measurements that systematically span most local times and latitudes, over a regular sampling of Mars seasons, and throughout the bottom half of the solar cycle. Such sampling will far surpass that available from existing spacecraft and ground-based datasets. In addition, remote measurements will provide a systematic mapping of the composition and structure of Mars neutral upper atmosphere and coronae (e.g. H, C, N, O), as well as probe lower altitudes. Such a detailed characterization is a necessary first step toward answering MAVEN's three main science questions (see Jakosky et al. 2014, this issue). This information will be used to determine present day escape rates from Mars, and provide an estimate of integrated loss to space throughout Mars history.

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“…The physics of the exosphere is interesting in that thermal escape , chemical-induced escape (De La Haye et al 2007b), slow hydrodynamic escape (Strobel 2008b), pick-up and ionospheric ion loss (Ledvina et al 2005;, and atmospheric sputtering ) have all been proposed as processes that are active at present . It is also interesting that atmospheric sputtering varies considerably depending on whether Titan is in Saturn's magnetosphere or exposed to the solar wind flux (Penz et al 2005).…”

Section: Titanmentioning

confidence: 99%