Mars gravity field based on a short-arc technique

Sjogren, W. L.; Lorell, J.; Wong, L.; Downs, W.

doi:10.1029/jb080i020p02899

Cited by 63 publications

(22 citation statements)

References 11 publications

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“…Gravity anomaly errors from GLGM-1 ranged from 22 milli-Galileos (mGal) (0.22 mm sp2 over the welltracked near side at low latitudes to 47 mGal for the high-latitude far side. W e evaluated the global gravitational field of the moon at the surface, rather than at spacecraft altitude as done by others (13,16,17). In comparison with the most recent pre-Clementine gravity model of Konopliv and colleagues ( 1 3), GLGM-1…”

Section: Free-air Gravitymentioning

confidence: 99%

The Shape and Internal Structure of the Moon from the Clementine Mission

Zuber

Smith

Lemoine

et al. 1994

Science

350

195

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Global topographic and gravitational field models derived from data collected by the Clementine spacecraft reveal a new picture of the shape and internal structure of the moon. The moon exhibits a 16-kilometer range of elevation, with the greatest topographic excursions occurring on the far side. Lunar highlands are in a state of near-isostatic compensation, whereas impact basins display a wide range of compensation states that do not correlate simply with basin size or age. A global crustal thickness map reveals crustal thinning under all resolvable lunar basins. The results indicate that the structure and thermal history of the moon are more complex than was previously believed.

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Section: Free-air Gravitymentioning

confidence: 99%

The Shape and Internal Structure of the Moon from the Clementine Mission

Zuber

Smith

Lemoine

et al. 1994

Science

350

195

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“…The gravity data for the Bouguer calculations are taken from low altitude line-of-sight (LOS) Doppler gravity observations of the Viking Orbiter II mission (Sjogren, 1979). These data can be considered as LOS free air gravity.…”

Section: Calculation Of Bouguer and Model Gravitiesmentioning

confidence: 99%

“…The highest resolution obtained by this method is of twelfth degree and order in gravity (Christensen and Balmino, 1979), i.e. Models of the Tharsis dome of Sleep and Phillips (1979) are based on a gravity field of Sjogren et al (1975) of l <~ 9. Regional and local model calculations are rare.…”

Section: Introductionmentioning

confidence: 99%

Bouguer gravity profiles across the highland-lowland escarpment on Mars

Janle

1983

The Moon and the Planets

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Selected Bouguer gravity profiles crossing the highland-lowland boundary of Mars are calculated. Density-depth models are presented for two areas. All profiles show an isostatic behaviour of the ancient highlands and the adjacent lowlands. Especially isostasy must be implied for the area of the escarpment. It is found that the whole Elysium dome is also nearly in isostatic equilibrium. These geophysical results and additional geological investigations imply a combination of subcrustal and minor surface erosion associated with relatively small vertical isostatic movements of the crust (sinking) in former highland areas. These processes caused a retreat of the highland escarpment of at least several hundred kilometers.* Contribution No. 254,

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“…Taking the coefficients determined by Sjogren et al (1975) and by Jordan & Lorell (1975) (Table 2) We may conclude that there is no indication here of a significant non-hydrostatic part of Ja.…”

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confidence: 92%

The moment of inertia of Mars and the existence of a core

Cook

1977

Geophysical Journal International

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A relation is obtained between the true value of the moment of inertia of a planet and the value calculated from the dynamical form factor, Jz, on the assumption of hydrostatic equilibrium. The result is applied to Mars and it is shown that the difference between the true and calculated moments of inertia is probably insignificant in considering models of the interior of Mars and in particular does not affect an argument for a core based on models calculated by Lyttleton.with the known value of the dynamical form factor, Jz (equal to (C --A)/Mu2) would allow C/Muz to be estimated. Thus it is necessary to derive C/Maz from Jz on the assumption that 350 A. H. Cook Mars is in hydrostatic equilibrium, using the formula derived (in effect) by Darwin (1899) c / M a z = 2 [I --( 2 4 m -3 J 2 )' "I 3 5 m + 3 J 2m is the ratio of the centrifugal to the gravitational acceleration at the equator. With J2 equal to 1.964 x the value of C/Maz is found to be 0.376, less than the minimum of Lyttleton's sequence of models. We infer (Cook 1972) that Mars is more centrally condensed than any of the mantle-type models and therefore that it contains a core of denser material, presumably more like the core of the Earth.With perhaps an indication of the presence of a core, this argument is not securely based. In the first place, it is now clear, as it was not when Lyttleton constructed his models, that there is not just a single change from upper to lower mantle in the Earth, but a complex transition which involves besides the olivine-spinel transition, changes in iron-magnesium ratio as well and possibly a final transition to a mixture of exides of which the lower mantle may be composed (see Binder & Davis 1973). Thus a sequence of models with a single transition radius is unlikely to be realistic and it might be thought that a much more elaborate set of models should be constructed.More serious, probably, is the fact that C/Maz has to be estimated from J2 making the

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Mars gravity field based on a short-arc technique

Cited by 63 publications

References 11 publications

The Shape and Internal Structure of the Moon from the Clementine Mission

The Shape and Internal Structure of the Moon from the Clementine Mission

Bouguer gravity profiles across the highland-lowland escarpment on Mars

The moment of inertia of Mars and the existence of a core

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