The question of an internal Martian magnetic field

Möhlmann, D.; Riedler, W.; Rustenbach, J.; Schwingenschuh, K.; Kurths, Jüergen; Motschmann, U.; Sauer, K.; Lichtenegger, H.

doi:10.1016/0032-0633(91)90130-3

Cited by 40 publications

(8 citation statements)

References 4 publications

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“…The hybrid or combined character of the solar wind interaction with Mars is also supported by the results of a spectral analysis of the Phobos-2 magnetic field data (Mohlmann et al, 1991) and the modulation of the tail diameter found in the plasma data (Verigin et al, 2001). The flaring of the Martian tail was investigated and it was found that the magnetotail is similar to the Earth's tail in its dependence on the pressure of the solar wind.…”

Section: Magnetic Field Topologymentioning

confidence: 95%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

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142

170

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Section: Magnetic Field Topologymentioning

confidence: 95%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

Self Cite

142

170

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“…MGS lacks ion measurements, and studies of the properties of these regions have necessarily focused on nightside magnetic field structure and superthermal electron distributions (each of which may indirectly provide clues about escaping particles and processes). The central wake and tail was also explored by Phobos, and its thickness and field orientation were used as support for both intrinsic and induced Martian obstacles to the solar wind (Riedler et al, 1989;Russell et al, 1995;Axford, 1991;Möhlmann et al, 1991;Dubinin et al, 1994). Comparison of MGS premapping MPB crossings to a model for the boundary shape by Verigin et al (2004) suggests that crustal magnetic fields act to make the tail boundary (the nightside extension of the MPB) thicker by up to 1000 km, so that both intrinsic and induced fields influence the tail structure.…”

Section: Wakementioning

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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“…The USSR's Phobos 2 mission provided observations as close as 800 km altitude. No conclusive evidence for a magnetic field of internal origin emerged (Riedler et al 1989), but some argued in favor of a small planetary field (Dolginov and Zhuzgov 1991;Slavin et al 1991;Moehlmann et al 1991) or localized magnetic anomalies (Moehlmann 1992). The controversy did not end until Mars Global Surveyor (MGS) entered Mars orbit in September 1997.…”

Section: Marsmentioning

confidence: 94%

Crustal Magnetic Fields of Terrestrial Planets

et al. 2009

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Magnetic field measurements are very valuable, as they provide constraints on the interior of the telluric planets and Moon. The Earth possesses a planetary scale magnetic field, generated in the conductive and convective outer core. This global magnetic field is superimposed on the magnetic field generated by the rocks of the crust, of induced (i.e. aligned on the current main field) or remanent (i.e. aligned on the past magnetic field). The crustal magnetic field on the Earth is very small scale, reflecting the processes (internal or external) that shaped the Earth. At spacecraft altitude, it reaches an amplitude of about 20 nT. Mars, on the contrary, lacks today a magnetic field of core origin. Instead, there is only a remanent magnetic field, which is one to two orders of magnitude larger than the terrestrial one at spacecraft altitude. The heterogeneous distribution of the Martian magnetic anomalies reflects the processes that built the Martian crust, dominated by igneous and cratering processes. These latter processes seem to be the driving ones in building the lunar magnetic field. As Mars, the Moon has no core-generated magnetic field. Crustal magnetic features are very weak, reaching only 30 nT at 30-km altitude. Their distribution is heterogeneous too, but the most intense anomalies are located at the antipodes of the largest impact basins. B. Langlais et al. The picture is completed with Mercury, which seems to possess an Earth-like, global magnetic field, which however is weaker than expected. Magnetic exploration of Mercury is underway, and will possibly allow the Hermean crustal field to be characterized. This paper presents recent advances in our understanding and interpretation of the crustal magnetic field of the telluric planets and Moon.

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The question of an internal Martian magnetic field

Cited by 40 publications

References 4 publications

The Plasma Environment of Mars

The Plasma Environment of Mars

Mars Global Surveyor Measurements of the Martian Solar Wind Interaction

Crustal Magnetic Fields of Terrestrial Planets

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