Magnetic field in the very close neighborhood of Mars according to data from the Mars 2 and Mars 3 spacecraft

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

doi:10.1029/ja078i022p04779

Cited by 119 publications

(33 citation statements)

References 9 publications

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“…Thus the shock position chosen by Dolginov et al (1973) stands off further than that given by Valsberg et al (at more than 2350 km instead of 1100 km at the subsolar position). Specifically, for the January 21 passage reported by both groups, in the region of magnetic fluctuations said to lie downstream of the shock, Valsberg et al (1973a) originally reported from the ion energy spectra that the plasma was supersonic and non-thermal.…”

Section: Discussionmentioning

confidence: 62%

“…(iii) The maxima of field and electron density reportedly do not coincide in space (Dolginov et al 1973). …”

Section: Discussionmentioning

confidence: 92%

“…A region of enhanced field penetrated by both the Mars-2 and Mars-3 probes in January 1972 at 2000-2500 km ahead of the planet was tentatively identified as the Martian magnetosphere (Dolginov, Yeroshenko & Zhuzgov 1973). Later passes through this region in April 1972 failed to detect the strongly enhanced field, which would be explained by an increased solar wind pressure at this time.…”

Section: Discussionmentioning

confidence: 95%

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Does Mars have a Magnetosphere?

Wallis

1975

Geophys J Int

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Section: Discussionmentioning

confidence: 62%

“…(iii) The maxima of field and electron density reportedly do not coincide in space (Dolginov et al 1973). …”

Section: Discussionmentioning

confidence: 92%

Section: Discussionmentioning

confidence: 95%

See 1 more Smart Citation

Does Mars have a Magnetosphere?

Wallis

1975

Geophys J Int

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“…Estimation of the magnetic moment depends on the interpretation of the observed magnetic fields. Dolginov et al (1973Dolginov et al ( , 1976 assumed that the magnetic fields observed with Mars 2, Mars 3 and Mars 5 spacecraft were influenced by an intrinsic magnetic field of Mars and concluded that the magnetic moment was of 2.4-2.5 × 10 22 G·cm 3 . On the other hand, Russell (1978a, b) claimed that magnetic fields observed by Mars-series spacecraft tend to be wrapped around the planet, and proposed an upper limit to the magnetic moment of 2 × 10 21 G·cm 3 .…”

Section: Intrinsic and Crustal Fieldmentioning

confidence: 99%

PLANET-B magnetic fields investigation

Yamamoto

Matsuoka

2014

Earth Planet Sp

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Some scientific topics relating to magnetic field measurements around Mars are briefly described and specification of the magnetic field instrument onboard PLANET-B is presented. The highly elliptical orbit of PLANET-B with a periapsis altitude of 150 km and an apoapsis of 15 R M (Mars radii) will enable us to observe magnetic environments in various regions from the ionospheric altitudes to upstream and tail regions. One of the most important objectives is to resolve the controversial arguments about the magnitude of the magnetic moment of Mars. Combination of measurements with other instruments onboard PLANET-B will give us important information on unsolved problems such as the pressure balance in the dayside ionosphere and acceleration processes for ionospheric ions.

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“…The obstacle to the solar wind flow at Mars has been observed for more than 45 years by several spacecraft. First crossings of the dayside magnetosphere with observations of increasing magnetic field up to ~30 nT (Dolginov et al, ) and ions of lower energy than magnetosheath ions were made by Mars 2 and Mars 3 (called then “ion cushion”; Bogdanov & Vaisberg, ). The ion and magnetic tail at ~7 R М with planetary ions outflow was found on Mars 5 (Dolginov, ; Vaisberg, ).…”

Section: Introductionmentioning

confidence: 99%

The Structure of Martian Magnetosphere at the Dayside Terminator Region as Observed on MAVEN Spacecraft

et al. 2018

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We analyzed 44 passes of the Mars Atmosphere and Volatile EvolutioN mission (MAVEN) spacecraft through the magnetosphere, arranged by the angle between electric field vector and the projection of spacecraft position radius vector in the plane perpendicular to the Mars‐Sun line (θE). All passes were divided into three angular sectors near 0°, 90°, and 180° θE angles in order to estimate the role of the interplanetary magnetic field direction in plasma and magnetic properties of dayside Martian magnetosphere. The time interval chosen was from 17 January to 4 February 2016 when MAVEN was crossing the dayside magnetosphere at solar zenith angle ~70°. Magnetosphere as the region with prevailing energetic planetary ions is always found between the magnetosheath and the ionosphere. The analysis of dayside interaction region showed that for each angular sector with different orientation of the solar wind electric field vector E = −1/c V × B one can find specific profiles of the magnetosheath, the magnetic barrier (Michel, 1971, https://doi.org/10.1029/RG009i002p00427; Zhang et al., 1991, https://doi.org/10.1029/91JA00088), and the magnetosphere. Magnetic barrier forms in front of the magnetosphere, and relative magnetic field magnitudes in these two domains vary. The average height of the boundary with ionosphere is ~530 km, and the average height of the magnetopause is ~730 km. We discuss the implications of the observed magnetosphere structure to the planetary ions loss mechanism.

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Magnetic field in the very close neighborhood of Mars according to data from the Mars 2 and Mars 3 spacecraft

Cited by 119 publications

References 9 publications

Does Mars have a Magnetosphere?

Does Mars have a Magnetosphere?

PLANET-B magnetic fields investigation

The Structure of Martian Magnetosphere at the Dayside Terminator Region as Observed on MAVEN Spacecraft

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