Structure of the martian wake

Fedorov, A.; Budnik, E.; Sauvaud, J. A.; Mazelle, C.; Barabash, S.; Lundin, R.; Acuña, M. H.; Holmström, Mats; Grigoriev, Alexander; Yamauchi, M.; Andersson, H.; Thocaven, J. J.; Winningham, D.; Frahm, R. A.; Sharber, J. R.; Scherrer, J.; Coates, A. J.; Linder, Dietmar; Kataria, D. O.; Kallio, Esa; Koskinen, H.; Säles, T.; Riihelä, P.; Schmidt, W.; Kozyra, J. U.; Luhmann, J. G.; Roelof, E. C.; Williams, D. J.; Livi, S.; Curtis, C. C.; Hsieh, K. C.; Sandel, B. R.; Grandé, M.; Carter, M.; McKenna-Lawler, S.; Orsini, S.; Cerulli-Irelli, R.; Maggi, M.; Würz, Peter; Bochsler, P.; Krupp, N.; Woch, J.; Fränz, M.; Asamura, Kazushi; Dierker, C.

doi:10.1016/j.icarus.2005.09.021

Cited by 88 publications

(76 citation statements)

References 25 publications

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“…In the simulations the MPB is also well identified from a jump in the magnetic field intensity. In addition, close to this boundary a change in the plasma composition occurs and planetary ions dominate downstream the MPB (Lundin et al, 1991;Dubinin et al, 1996;Modolo et al, Fedorov et al, 2006). Figure 1 clearly displays the MPB and, similar to the BS features, a strong asymmetry is marked in the XY plane while the XZ plane is nearly symmetric.…”

Section: The Mpbmentioning

confidence: 84%

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

Modolo

Chanteur²,

Dubinin³

et al. 2006

Ann. Geophys.

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Abstract. The solar wind plasma interaction with the Martian exosphere is investigated by means of 3-D multi-species hybrid simulations. The influence of the solar EUV flux on the bow shock and the magnetic pile-up boundary is examined by comparing two simulations describing the two extreme states of the solar cycle. The hybrid formalism allows a kinetic description of each ions species and a fluid description of electrons. The ionization processes (photoionization, electron impact and charge exchange) are included self-consistently in the model where the production rate is computed locally, separately for each ionization act and for each neutral species. The results of simulations are in a reasonable agreement with the observations made by Phobos 2 and Mars Global Surveyor spacecraft. The position of the bow shock and the magnetic pile-up boundary is weakly dependent of the solar EUV flux. The motional electric field creates strong asymmetries for the two plasma boundaries.

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Section: The Mpbmentioning

confidence: 84%

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

Modolo

Chanteur²,

Dubinin³

et al. 2006

Ann. Geophys.

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“…This situation is more realistic. The IMF y and z components of the Parker IMF case were derived from Mars Global Surveyor (MGS) data, recorded on February 27, 2004, with the method used by Fedorov et al (2006). The draped IMF measured by MGS is expected to have the same orientation in the y-z plane as the upstream IMF (Brain et al, 2006;Fedorov et al, 2006).…”

Section: Input Parameters: Solar Windmentioning

confidence: 99%

Hybrid simulations of proton precipitation patterns onto the upper atmosphere of Mars

et al. 2012

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We study the dependence of proton precipitation patterns onto the Martian upper atmosphere on altitude, proton energy, proton origin, and in a lesser extent, solar zenith angle, using the HYB-Mars model, a 3D quasineutral hybrid model. We find that the flux of precipitating protons has a strong altitude dependence: on the dayside, the flux of precipitating protons decreases substantially when the altitude over Mars decreases. We also find that the contribution of exospheric protons to the deposition is significant and its spatial distribution is not identical to that of the solar wind protons. In addition, the low energy proton population comes mainly from the newborn planetary protons. The energized pick-up protons and solar wind protons contribute to the higher energy proton population. The study also confirms that the proton precipitation is highly asymmetric with respect to the direction of the convection electric field in the solar wind. The study implies that the Martian induced magnetosphere protects the upper atmosphere effectively against proton precipitation.

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“…Figure 2 shows maps of electron fluxes for the Northern dayside Hemisphere (where effects of crustal fields are small) for different signs of the B y component of the IMF. A proxy direction of the B yIMF component was inferred from the MGS observations assuming that the magnetic field at middle latitudes of the Northern Hemisphere is primarily of induced origin (Brain et al, 2006b;Dubinin et al, 2006;Fedorov et al, 2006). A positive sign corresponds to the case when piled up magnetic field is expected to be higher in the Northern Hemisphere.…”

Section: Access Of Solar Wind Electrons On the Daysidementioning

confidence: 99%

Access of solar wind electrons into the Martian magnetosphere

et al. 2008

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Abstract. Electrons with energy of ∼40-80 eV measured by the instrument ASPERA-3 on Mars Express and MAG-ER onboard Mars Global Surveyor are used to trace an access of solar wind electrons into the Martian magnetosphere. Crustal magnetic fields create an additional protection from solar wind plasma on the dayside of the Southern Hemisphere by shifting the boundary of the induced magnetosphere (this boundary is often refereed as the magnetic pileup boundary) above strong crustal sources to ∼400 km as compared to the Northern Hemisphere. Localized intrusions through cusps are also observed. On the nightside an access into the magnetosphere depends on the IMF orientation. Negative values of the B yIMF component assist the access to the regions with strong crustal magnetizations although electron fluxes are strongly weakened below ∼600 km. A precipitation pattern at lower altitudes is formed by intermittent regions with reduced and enhanced electron fluxes. The precipitation sites are longitudinally stretched narrow bands in the regions with a strong vertical component of the crustal field. Fluxes ≥10 9 cm −2 s −1 of suprathermal electrons necessary to explain the observed aurora emissions are maintained only for the periods with enhanced precipitation. The appearance of another class of electron distributions -inverted V structures, characterized by peaks on energy spectra, is controlled by the IMF. They are clustered in the hemisphere pointed by the interplanetary electric field that implies a constraint on their origin.

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Structure of the martian wake

Cited by 88 publications

References 25 publications

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

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

Hybrid simulations of proton precipitation patterns onto the upper atmosphere of Mars

Access of solar wind electrons into the Martian magnetosphere

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