The solar wind interaction with Mars: Consideration of Phobos 2 mission observations of an ion composition boundary on the dayside

Бреус, Т. К.; Крымский, А. М.; Lundin, R.; Dubinin, E.; Luhmann, J. G.; Yeroshenko, Ye.; Barabash, S. V.; Mitnitskii, V.Ya.; Pissarenko, N. F.; Styashkin, V. A.

doi:10.1029/91ja01131

Cited by 70 publications

(53 citation statements)

References 31 publications

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“…They were introduced as the magnetopause (Rosenbauer et al, 1989;Lundin et a!., 1989), the Protonopause (Sauer et al, 1994 ), and the ion composition boundary (Breus et al, 1991). However, one significant handicap that the Phobos-2 mission suffered under was the large spacecraft periapsis altitude of about 850 km above the surface.…”

mentioning

confidence: 99%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

142

170

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mentioning

confidence: 99%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

142

170

View full text Add to dashboard Cite

“…Ion measurements conducted by the ASPERA and HARP experiments aboard Phobos-2 identified an Ion Composition Boundary (ICB) which was located at the same position as the magnetic pile-up boundary (MPB). This boundary separates the solar wind protons from the planetary ions (Sauer et al, 1990;Breus et al, 1991;Sauer et al, 1994). The magnetic pile-up boundary at Mars has been observed between the bow shock and the ionopause by both Mars Global Surveyor and the Phobos-2 MAGMA instrument (Riedler et al, 1991;Vignes et al, 2000).…”

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confidence: 99%

Physics of the Ion Composition Boundary: a comparative 3-D hybrid simulation study of Mars and Titan

et al. 2007

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Abstract. The plasma environments of Mars and Titan have been studied by means of a 3-D hybrid simulation code, treating the electrons as a massless, charge-neutralizing fluid, whereas ion dynamics are covered by a kinetic approach. As neither Mars nor Titan possesses a significant intrinsic magnetic field, the upstream plasma flow interacts directly with the planetary ionosphere. The characteristic features of the interaction region are determined as a function of the alfvénic, sonic and magnetosonic Mach number of the impinging plasma. For the Martian interaction with the solar wind as well as for the case of Titan being located outside Saturn's magnetosphere in times of high solar wind dynamic pressure, all three Mach numbers are larger than 1. In such a scenario, the interaction gives rise to a so-called Ion Composition Boundary, separating the ionospheric plasma from the ambient flow and being highly asymmetric with respect to the direction of the convective electric field. The formation of these features is explained by analyzing the Lorentz forces acting on ionospheric and ambient plasma particles. Titan's plasma environment is highly variable and allows various different combinations of the three Mach numbers. Therefore, the Ion Composition Boundary may vanish under certain circumstances. The relevant physical mechanism is illustrated as a function of the Mach numbers in the upstream plasma flow.

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“…Therefore, the solar wind is decelerated upstream of the obstacle, leading to the formation of a bow shock. In both cases the supersonic solar wind is expected to be separated from the ionospheric heavy ion population by an ion composition boundary, as initially reported by Breus et al (1991) and Sauer et al (1994). The physics of this boundary layer have already been extensively studied within the framework of numerical models such as the approaches by Sauer and Dubinin (2000), Bößwetter et al (2004), Simon et al (2007a), and Bößwetter et al (2007).…”

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confidence: 85%

Rosetta swing-by at Mars – an analysis of the ROMAP measurements in comparison with results of 3-D multi-ion hybrid simulations and MEX/ASPERA-3 data

et al. 2009

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Abstract. The Rosetta spacecraft flew by Mars at a distance of 260 km on 25 February 2007 during a gravity assist manoeuvre. During the closest approach (CA) the lander magnetometer ROMAP was switched on. The dataset taken during this swingby provides insight into the plasma environment around Mars: in addition to a pronounced bow shock crossing Rosetta recorded the signature of the pile up region of draped magnetic field. Also the Rosetta measurements showed signatures of crustal magnetic field anomalies which can be verified by results of a crustal magnetic field model. In order to understand the measured field morphology, multi-ion hybrid simulations were performed. Some of the input parameters for the simulations were obtained from Mars Express (MEX) data which were contemporaneously collected during the Rosetta swingby. These simulations reproduces ROMAP magnetic field measurements and show that the interplanetary magnetic field pointed northward during the encounter. A spectral analysis shows upstream waves ahead of the bow shock and indicates the presence of the magnetic pile-up boundary (MPB). The multi-ion model reproduces the ion fluxes measured by MEX/ASPERA-3 and is in agreement with the measurements to within one order of magnitude.

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The solar wind interaction with Mars: Consideration of Phobos 2 mission observations of an ion composition boundary on the dayside

Cited by 70 publications

References 31 publications

The Plasma Environment of Mars

The Plasma Environment of Mars

Physics of the Ion Composition Boundary: a comparative 3-D hybrid simulation study of Mars and Titan

Rosetta swing-by at Mars – an analysis of the ROMAP measurements in comparison with results of 3-D multi-ion hybrid simulations and MEX/ASPERA-3 data

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