Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...123..225d&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 123, no. 2, July 1983, p. 225-237.
Astronomy and Astrophysics
Astrophysics
13
Mars Surface Samples, Mars 5 Spacecraft, Planetary Surfaces, Soil Science, Albedo, Mars Atmosphere, Polarized Light, Remote Sensing, Surface Properties, Textures, Mars, Surface, Texture, Soils, Mars-5, Photopolarimetery, Procedure, Polarization, Argyre Quadrangles, Thaumasia Quadrangle, Wavelengths, Analysis, Comparisons, Deposits, Eolian Features, Winds, Distribution, Size, Terrain, Claritas Fossae, Thaumasia Fossae, Soils, Ogygis Rupes, Grains, Data
Scientific paper
The highest values of the degree of polarization, which occur around a phase angle of 100 deg, together with the albedos, are determined for a large number of small areas at the surface of Mars. They are interpreted in terms of Martian soil microtexture on the basis of a comparative analysis with lunar, terrestrial, meteoritic, and artificial samples. Despite the great variety of the Martian terrain and the geomorphological units analyzed, the surface of Mars at the scale of tens of kilometers appears everywhere as a finely or even very finely pulverized soil. The regions covered by eolian deposits characterized by wind streaks and splotches are generally finely divided, as on the lunar surface. The grain-size distribution can be characterized by approximately half of the cumulative weight diameters smaller than 40 microns; it is comparable to terrestrial loess rather than sand dunes. The fractured terrains processed by tectonic activities (Claritas Fossae, Thaumasia Fossae, and Ogygis Rupes) are found to have a coarser soil that includes larger grains or rocks.
Deschamps M.
Dollfus Audouin
Ksanfomaliti L. V.
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