Observations of the latitude dependence of the location of the martian magnetic pileup boundary

Crider, D. H.; Acuña, M. H.; Connerney, J. E. P.; Vignes, D.; Ness, N. F.; Крымский, А. М.; Бреус, Т. К.; Rème, H.; Mazelle, C.; Mitchell, David; Lin, R. P.; Cloutier, P. A.; Winterhalter, D.

doi:10.1029/2001gl013860

Cited by 113 publications

(93 citation statements)

References 11 publications

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“…It is worth noting that the model of the MB position based both on MGS and Phobos-2 observations (Trotignon et al, 2006) gives a reasonable agreement with the above mentioned models. It is seen that the MB moves upward in the Southern Hemisphere (dashed curve) that is in the agreement with the MGS observations (Crider et al, 2002). At solar zenith angles SZA≥45 • the shift reaches ∼500 km.…”

Section: Access Of Solar Wind Electrons On the Daysidesupporting

confidence: 77%

“…The boundary has been often refereed as the magnetic pileup boundary (Bertucci et al, 2003;Nagy et al, 2004). Crustal magnetic fields can contribute to the total pressure of the obstacle against the solar wind (Crider et al, 2002;Dubinin et al, 2006). Average positions of the bow shock (BS) and the magnetospheric boundary (MB) determined, respectively, from the MGS and MEX observations (Vignes et al, 2000;Dubinin et al, 2006) are also shown.…”

Section: Access Of Solar Wind Electrons On the Daysidementioning

confidence: 99%

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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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Section: Access Of Solar Wind Electrons On the Daysidesupporting

confidence: 77%

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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“…Crider et al (2002) have found that the magnetospheric boundary moves upward with increasing southern latitude. Fraenz et al (2006) and Dubinin et al (2008a) have shown that the boundary above strong crustal sources can shift upward by ∼400 km as compared to the boundary in the northern hemisphere.…”

Section: Discussionmentioning

confidence: 99%

Upper ionosphere of Mars is not axially symmetrical

et al. 2012

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The measurements carried out by the ASPERA-3 and MARSIS experiments on board the Mars Express (MEX) spacecraft show that the upper Martian ionosphere (h ≥ 400 km) is strongly azimuthally asymmetrical. There are several factors, e.g., the crustal magnetization on Mars and the orientation of the interplanetary magnetic field (IMF) which can give rise to formation of ionospheric swells and valleys. It is shown that expansion of the ionospheric plasma along the magnetic field lines of crustal origin can produce bulges in the plasma density. The absense of a magnetometer on MEX makes the retrieval of an asymmetry caused by the IMF more difficult. However hybrid simulations give a hint that the ionosphere in the hemisphere (E − ) to which the motional electric field is pointed occurs more inflated than the ionosphere in the opposite (E + ) hemisphere.

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“…The crustal magnetic field will be included in a future study, with an improved spatial resolution of 150 km accompanied with a better description of the ionosphere. Note here that Crider et al (2002) and Dubinin et al (2006) 1 have reported a dependence of the MPB position on the presence of crustal fields.…”

Section: The Mpbmentioning

confidence: 95%

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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Observations of the latitude dependence of the location of the martian magnetic pileup boundary

Cited by 113 publications

References 11 publications

Access of solar wind electrons into the Martian magnetosphere

Access of solar wind electrons into the Martian magnetosphere

Upper ionosphere of Mars is not axially symmetrical

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

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