Preliminary Radar Results of Mars

Goldstein, Robert S.; Melbourne, W. G.; Morris, G. A.; Downs, G. S.; O'Handley, Douglas A.

doi:10.1029/rs005i002p00475

Cited by 29 publications

(4 citation statements)

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“…Observations of the Martian topography have been attempted by many investigators (Belton and Hunten, 1969;Pettengill et al, 1969;Pollack and Sagan, 1969;Wells, 1969;Goldstein et al, 1970;Rogers et al, 1970;Woszczyk, 1971). Some of their results are reproduced in Figs.…”

Section: Topography Of Marssupporting

confidence: 50%

The Dynamical Effects of Real Mars Orography upon the Large-scale Air Flow and Some Meteorological Phenomena of Mars

Moriyama

1973

Journal of the Meteorological Society of Japan

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Numerical experiments are performed to investigate to what extent the observed features are explained in terms of the dynamical modification of air flow by the realistic Mars topography. The real Mars topography based on radar-and optical observations is incorporated in the fully non-linear shallow water equations with realistic Coriolis parameter. These equations are integrated numerically as an initial and boundary value problem for air flow across mountain.Comparison of results with the observed data shows the following; 1) In spite of a limitation that the baroclinic effect is ignored, the quasi-stationary troughs and ridges are realized and they are highly in agreement with observed circulation patterns. This result endorses that the observed permanent low or steady flow on Mars appears under the strong influence of orography.2) The present numerical experiments also suggest that in the northern hemisphere, north winds intensified by orography would be considerably responsible for the courses of "darkening waves" .

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Section: Topography Of Marssupporting

confidence: 50%

The Dynamical Effects of Real Mars Orography upon the Large-scale Air Flow and Some Meteorological Phenomena of Mars

Moriyama

1973

Journal of the Meteorological Society of Japan

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“…The volcanic deposits forming the Syrtis Major shield spread over the cratered plateau west of the Isidis basin and into that depression in at least two eruptive stages. The first stage is represented by the extensive ridged-plains unit that now dominates the surface of the shield (Figure 1 [ Sagan, 1967, 1970;Hunten, 1969, 1971;Wells, 1969;Goldstein et al, 1970;Rogers et al, 1970;Sagan et al, 1971;Frey, 1974]. Although Syrtis Major is historically one of the most persistent dark features on Mars, seasonal changes in its overall appearance were first described by Antoniadi [1930] and later verified by Slipher [ 1962].…”

Section: Syrtis Major Shield (Figures 1-3) the Larger Caldera (C•) Imentioning

confidence: 99%

Syrtis major: A low‐relief volcanic shield

Schaber¹

1982

J. Geophys. Res.

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Viking orbiter images and earth‐based radar elevation data have been used to document the volcanic geology of Syrtis Major and to reevaluate its physiographic setting. These data indicate that Syrtis Major is actually a very low relief, simple shield with a central caldera complex; arcuate segments of concentric grabens at the shield summit define the limits of a 280‐km‐diameter depression that is thought to have been created by foundering of a magma chamber. Lava flows with well‐defined scarps are associated with two summit calderas; fissures and lava tubes are recognized on the shield flanks. The lava flows were deposited on volcanic ridged plains that do not display flow scarps. Compressional stresses acting on the shield were apparently greatest following the deposition of the ridged‐plains unit but continued at a somewhat reduced rate after deposition of the younger lavas. The extremely low‐relief shield of the Syrtis Major as well as other volcanic plains of intermediate age in the eastern hemisphere of Mars is in striking contrast to the giant shields of Tharsis Montes. Such different types of volcanic landforms may result from changes with times in the composition, differentiation history, eruption rates, and eruption temperatures of surface igneous rocks, thus, directly reflecting the thermal and chemical evolution of the interior. The low relief on the shields may also reflect a substantially thinner crust in these regions relative to Tharsis. The physiographic evidence and radar elevation data confirm the fact that Syrtis Major is a ‘planum’ (plateau) rather than a ‘planitia’ (low plain), as published maps of Mars now portray the feature. In addition, present evidence does not support an earlier suggestion that an impact basin predated volcanism at Syrtis Major.

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“…During most of the recent Mars oppositions, beginning with the 1969 opposition, Mars has been the target of radar ranging experiments carried out at the NASA's Goldstone radar observatory (Goldstein et al, 1970;Downs et al, 1971Downs et al, ,1973Downs et al, ,1975Downs et al, ,1978Downs et al, ,1982. The experiment resulted in acquisition of radar altimetric data for planet's equatorial region.…”

Section: Earth-based Radar Altimetry Of Marsmentioning

confidence: 99%

Schroeter's ratios for Martian craters: Radar results

Roth

1991

Earth Moon Planet

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Schroeter's ratios (ratios of the rim volume to the apparent volume) are determined for a sample of 29 large, degraded Martian craters selected from the Goldstone Mars radar altimetry data. On the average, the values of the calculated Schroeter's ratios are about two orders of magnitude smaller than the same ratios for fresh lunar craters. This indicates a severe rim volume deficit in degraded Martian craters and it provides an additional support to the notion of a widespread resurfacing of intercrater plains on Mars. Schroeter's ratios for degraded craters could provide a semi-quantitative measure of the effects of the modification processes that had been active on Mars and on the other planetary bodies.

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Preliminary Radar Results of Mars

Abstract: Radar studies of Mars during the 1969 opposition (not yet completed) have yielded preliminary results. Elevation and radar brightness is presented as a function of longitude forareas between 3 ø and 12ø north latitude.

Cited by 29 publications

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The Dynamical Effects of Real Mars Orography upon the Large-scale Air Flow and Some Meteorological Phenomena of Mars

The Dynamical Effects of Real Mars Orography upon the Large-scale Air Flow and Some Meteorological Phenomena of Mars

Syrtis major: A low‐relief volcanic shield

Schroeter's ratios for Martian craters: Radar results

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