The magnetic field of mars according to the data from the Mars 3 and Mars 5

Dolginov, Sh. Sh.; Yeroshenko, Ye.; Zhuzgov, L. N.

doi:10.1029/ja081i019p03353

Cited by 66 publications

(14 citation statements)

References 11 publications

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“…Then the motional electric field E = −V sw × B IMF is always along the Z -axis. Such a system was successfully used in previous studies (Dolginov et al 1981;Saunders and Russell 1986;Yeroshenko et al 1990;Dubinin et al 1996b). Since there is no magnetometer on MEX the only way to get information about the IMF was the Mars Global Surveyor (MGS) measurements at the dayside, at 400 km altitude.…”

Section: Momentum Conservation Constraints and Global Morphology Of Ementioning

confidence: 86%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

162

174

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Mars and Venus do not have a global magnetic field and as a result solar wind interacts directly with their ionospheres and upper atmospheres. Neutral atoms ionized by solar UV, charge exchange and electron impact, are extracted and scavenged by solar wind providing a significant loss of planetary volatiles. There are different channels and routes through which the ionized planetary matter escapes from the planets. Processes of ion energization driven by direct solar wind forcing and their escape are intimately related. Forces responsible for ion energization in different channels are different and, correspondingly, the effectiveness of escape is also different. Classification of the energization processes and escape channels on Mars and Venus and also their variability with solar wind parameters is the main topic of our review. We will distinguish between classical pickup and 'massloaded' pickup processes, energization in boundary layer and plasma sheet, polar winds on unmagnetized planets with magnetized ionospheres and enhanced escape flows from localized auroral regions in the regions filled by strong crustal magnetic fields.

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Section: Momentum Conservation Constraints and Global Morphology Of Ementioning

confidence: 86%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

162

174

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“…From 1971 to 1974 the Soviet Mars missions (2, 3, 5) also measured the bow shock and the underlying sheath using magnetometers and ion and electron instruments (e.g. Bogdanov and Vaisberg, 1975;Dolginov et al, 1976). Additionally, they made the first measurements of the "ion cushion", identified in Figure 1 as the MPR.…”

Section: Introductionmentioning

confidence: 99%

Mars Global Surveyor Measurements of the Martian Solar Wind Interaction

Brain

2006

Space Sci Rev

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The solar wind at Mars interacts with the extended atmosphere and small-scale crustal magnetic fields. This interaction shares elements with a variety of solar system bodies, and has direct bearing on studies of the long-term evolution of the Martian atmosphere, the structure of the upper atmosphere, and fundamental plasma processes. The magnetometer (MAG) and electron reflectometer (ER) on Mars Global Surveyor (MGS) continue to make many contributions toward understanding the plasma environment, thanks in large part to a spacecraft orbit that had low periapsis, had good coverage of the interaction region, and has been long-lived in its mapping orbit. The crustal magnetic fields discovered using MGS data perturb plasma boundaries on timescales associated with Mars' rotation and enable a complex magnetic field topology near the planet. Every portion of the plasma environment has been sampled by MGS, confirming previous measurements and making new discoveries in each region. The entire system is highly variable, and responds to changes in solar EUV flux, upstream pressure, IMF direction, and the orientation of Mars with respect to the Sun and solar wind flow. New insights from MGS should come from future analysis of new and existing data, as well as multi-spacecraft observations.

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“…Phobos and Deimos (dust rings) Ip, 1988;Dubinin et al ., 1990;Barabash and Lundin, 1994 dust counter, all plasma B, waves, Camera Intrinsic B-field Riedler et al ., 1989;Dolginov et al ., 1976;Yeroshenko et al ., 1990 B all plasma …”

Section: Scientific Objectivesmentioning

confidence: 99%