Oxygen outflow in the Martian magnetotail

Kallio, Esa; Koskinen, Hannu E. J.; Barabash, S.; Nairn, C. M. C.; Schwingenschuh, K.

doi:10.1029/95gl02474

Cited by 36 publications

(34 citation statements)

References 17 publications

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“…In a very detailed IMA data -QNH model comparison the energy spectra should be generated by using the positions of MEX, the attitudes of IMA instrument, and the accurate IMA FOV but this is beyond the present study. Kallio et al, 1995). Also ASPERA-3/MEX has measured ∼1 keV planetary ions in the nightside (see, for example, Kallio et al, 2006, Figure 1).…”

Section: Similarities With Observationsmentioning

confidence: 97%

Energisation of O+ and O+ 2 Ions at Mars: An Analysis of a 3-D Quasi-Neutral Hybrid Model Simulation

et al. 2006

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We have studied the loss of O + and O + 2 ions at Mars with a numerical model. In our quasi-neutral hybrid model ions (H + , He ++ , O + , O + 2 ) are treated as particles while electrons form a massless charge-neutralising fluid. The employed model version does not include the Martian magnetic field resulting from the crustal magnetic anomalies. In this study we focus the Martian nightside where the ASPERA instrument on the Phobos-2 spacecraft and recently the ASPERA-3 instruments on the Mars Express spacecraft have measured the proprieties of escaping atomic and molecular ions, in particular O + and O + 2 ions. We study the ion velocity distribution and how the escaping planetary ions are distributed in the tail. We also create similar types of energyspectrograms from the simulation as were obtained from ASPERA-3 ion measurements. We found that the properties of the simulated escaping planetary ions have many qualitative and quantitative similarities with the observations made by ASPERA instruments. The general agreement with the observations suggest that acceleration of the planetary ions by the convective electric field associated with the flowing plasma is the key acceleration mechanism for the escaping ions observed at Mars.

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Section: Similarities With Observationsmentioning

confidence: 97%

Energisation of O+ and O+ 2 Ions at Mars: An Analysis of a 3-D Quasi-Neutral Hybrid Model Simulation

et al. 2006

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“…Two of the three main O + ion populations reported by Kallio et al (1995) are also modeled by the simulations: the shadow O + ions and the pick up O + ions. The energetic O + ions (E > 5 keV) found in the direction opposite to the motional electric field are believed to be associated with fluctuating electric and magnetic fields and cannot be reproduced within the framework of the present model.…”

Section: Ion Energeticsmentioning

confidence: 99%

“…The values of ions fluxes in the plasma sheet were in reasonable agreement with observations. Kallio et al (1995) have studied the distribution of O + -ions with different energies in the Martian magnetotail. They observed a steady population of oxygen ions in the shadow of the planet and attributed it to the asymmetric and dynamic plasmasheet.…”

Section: Introductionmentioning

confidence: 99%

Model calculations of the planetary ion distribution in the Martian tail

Lichtenegger

Dubinin

2014

Earth Planet Sp

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Based on a recent model of the Martian atmosphere/exosphere and a model of the magnetic field and solar wind flow around Mars, the distribution of different planetary ion species in the near tail is calculated. Three main regions are identified: 1) "clouds" of pickup ions with distinct mass separation travel along cycloidal trajectories; 2) another group of ions forms a distinct plasma mantle in the magnetosphere; 3) a third population fills up the plasma sheet. Further, the energy of ions in different locations is also analyzed. Finally, comparison of observations made onboard the Phobos-2 spacecraft shows a reasonable agreement with simulation results.

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“…The central tail has a plasma sheet containing oxygen streaming away from the planet that orients itself according to E SW (Dubinin et al, 1991). And oxygen ions in the outer night side tail measured by the ASPERA instrument on Phobos were interpreted by Kallio et al (1995) as escaping planetary pickup ions accelerated in the direction of E SW .…”

Section: Introductionmentioning

confidence: 99%