Ions of planetary origin in the Martian magnetosphere (Phobos 2/TAUS experiment)

Веригин, М. И.; Shutte, N. M.; Galeev, A. A.; Gringauz, K. I.; Котова, Г. А.; Remizov, A. P.; Rosenbauer, H.; Hemmerich, Peter; Livi, S.; Richter, A. K.; Apáthy, I.; Szegö, K.; Riedler, W.; Schwingenschuh, K.; Steller, M.; Yeroshenko, Ye.

doi:10.1016/0032-0633(91)90135-w

Cited by 103 publications

(69 citation statements)

References 12 publications

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“…On the other hand, photoionization is the main process which contributes to the escape of O + ions, which maximizes at solar maximum with the extension of oxygen corona. The loss rate of oxygen ions is about ten times smaller than the value given by Lundin et al (1990a) from the ASPERA measurements ( 2.5×10 25 ions/s) and is in better agreement with the estimates by Verigin et al (1991) equal to 5×10 24 ions/s from the TAUS measurements on board Phobos-2. The different assumptions made about the distribution of ion fluxes in the Martian tail explain this discrepancy between experimentals estimations.…”

Section: Estimation Of the Ionic Escapesupporting

confidence: 81%

Influence of the solar EUV flux on the Martian plasma environment

Modolo¹,

Chanteur²,

et al. 2005

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Abstract. The interaction of the solar wind with the Martian atmosphere and ionosphere is investigated by using threedimensional, global and multi-species hybrid simulations. In the present work we focus on the influence of the solar EUV flux on the Martian plasma environment by comparing simulations done for conditions representative of the extrema of the solar cycle. The dynamics of four ionic species (H + , He ++ , O + , O + 2 ), originating either from the solar wind or from the planetary plasma, is treated fully kinetically in the simulation model in order to characterize the distribution of each component of the plasma, both at solar maximum and at solar minimum. The solar EUV flux controls the ionization frequencies of the exospheric species, atomic hydrogen and oxygen, as well as the density, the temperature, and thus the extension of the exosphere. Ionization by photons and by electron impacts, and the main charge exchange reactions are self-consistently included in the simulation model. Simulation results are in reasonable agreement with the observations made by Phobos-2 and Mars Global Surveyor (MGS) spacecraft: 1) the interaction creates a cavity, void of solar wind ions (H + , He ++ ), which depends weakly upon the phase of the solar cycle, 2) the motional electric field of the solar wind flow creates strong asymmetries in the Martian environment, 3) the spatial distribution of the different components of the planetary plasma depends strongly upon the phase of the solar cycle. The fluxes of the escaping planetary ions are computed from the simulated data and results for solar maximum are compared with estimates based on the measurements made by experiments ASPERA and TAUS on board Phobos-2.

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Section: Estimation Of the Ionic Escapesupporting

confidence: 81%

Influence of the solar EUV flux on the Martian plasma environment

Modolo¹,

Chanteur²,

et al. 2005

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“…These published values were nearly two orders of magnitude lower than earlier estimates based on data from observations obtained with instruments from the Phobos spacecraft [Lundin et al, 1989;Rosenbauer et al, 1989;Verigin et al, 1991]. Therefore it is timely to again look at model calculations of these fluxes.…”

Section: Introductionmentioning

confidence: 67%

Ion escape fluxes from Mars

Nagy

2007

Geophysical Research Letters

111

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[1] A 3D, multi-species, non-ideal MHD numerical code was used to calculate the ion escape fluxes from Mars. The calculations were carried out for six cases with different nominal solar wind, solar cycle and crustal field orientation conditions and the total escape fluxes (the sum of the three major ionospheric species, O + , O 2 + , and CO 2 + ) varied by about an order of magnitude from 2.7 Â 10 23 to 2.4 Â 10 24 sec À1 . These results were compared to the recently measured Mars Express results of 3.2 Â 10 23 sec À1 (O + , O 2 + , and CO 2 + ), which were obtained near solar cycle minimum conditions, indicating a good agreement between measured and calculated fluxes. We also calculated the escape flux for ''extremely'' high solar wind conditions which leads to a flux of 3 Â 10 25 sec À1 .

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“…In Lundin et al [2013], they reported that the average heavy ion escape rate is increased by a factor of ∼10, from ∼1 ×10 24 s −1 (solar minimum) to ∼1 ×10 25 s −1 (solar maximum). On the other hand, both Verigin et al [1991] (by Phobos-2 observations) and Nilsson et al [2011] suggested that high solar activity leads to ∼2.5 times higher ion escape rate than the low solar activity result.…”

Section: Introductionmentioning

confidence: 99%

Solar wind interaction with the Martian upper atmosphere: Crustal field orientation, solar cycle, and seasonal variations

Dong

Bougher

et al. 2015

JGR Space Physics

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A comprehensive study of the solar wind interaction with the Martian upper atmosphere is presented. Three global models: the 3‐D Mars multifluid Block Adaptive Tree Solar‐wind Roe Upwind Scheme MHD code (MF‐MHD), the 3‐D Mars Global Ionosphere Thermosphere Model (M‐GITM), and the Mars exosphere Monte Carlo model Adaptive Mesh Particle Simulator (M‐AMPS) were used in this study. These models are one‐way coupled; i.e., the MF‐MHD model uses the 3‐D neutral inputs from M‐GITM and the 3‐D hot oxygen corona distribution from M‐AMPS. By adopting this one‐way coupling approach, the Martian upper atmosphere ion escape rates are investigated in detail with the combined variations of crustal field orientation, solar cycle, and Martian seasonal conditions. The calculated ion escape rates are compared with Mars Express observational data and show reasonable agreement. The variations in solar cycles and seasons can affect the ion loss by a factor of ∼3.3 and ∼1.3, respectively. The crustal magnetic field has a shielding effect to protect Mars from solar wind interaction, and this effect is the strongest for perihelion conditions, with the crustal field facing the Sun. Furthermore, the fraction of cold escaping heavy ionospheric molecular ions [( and/or )/Total] are inversely proportional to the fraction of the escaping (ionospheric and corona) atomic ion [O+/Total], whereas and ion escape fractions show a positive linear correlation since both ion species are ionospheric ions that follow the same escaping path.

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Ions of planetary origin in the Martian magnetosphere (Phobos 2/TAUS experiment)

Cited by 103 publications

References 12 publications

Influence of the solar EUV flux on the Martian plasma environment

Influence of the solar EUV flux on the Martian plasma environment

Ion escape fluxes from Mars

Solar wind interaction with the Martian upper atmosphere: Crustal field orientation, solar cycle, and seasonal variations

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