Wrinkle ridges are features created by compressive tectonic forces within the maria. The cratering rates are low. The surface has also experienced space weathering due to high energy particles, solar wind implantation, and micrometeorite impacts. This was confirmed by Chandra ACIS observations in 2001 (see Fig. Contours are at 42 K intervals (10% of maximum), except for the lowest contour, which is at 8 K (dashed contours are negative). As we just saw, the most densely cratered surfaces formed prior to 3.8 billion years ago, and the cratering rate has been roughly constant since that time. (See Fig. Craters provide a means of estimating the ages of surfaces. Venus and Mars have atmospheres which consist of over 95% carbon dioxide gas (CO2). [From Bhardwaj et al., 2002, ESA-SP-514, 215–226.]
J., 607, 596–610.] This erosional process softens and rounds the features of the crater. These areas could be more mafic volcanic pyroclastic deposits. A large portion of maria erupted within, or flowed into, the low-lying impact basins on the lunar nearside. The green dotted curve is the detector background. Lunar meteorites represent random (but unknown) impact sites. The day side lunar emissions are thought to be primarily reflected and fluoresced sunlight, while the faint night side emissions are foreground due to charge exchange of solar wind heavy ions with H atoms in Earth's exosphere. In particular, the largest impact basins were formed during the early periods, and these were successively overlaid by smaller craters. Nevertheless, by counting craters, we can put surfaces in a time-ordered sequence and make rough estimates of their absolute ages.
One of the most notable sinuous rilles is the Vallis Schröteri feature, located in the Aristarchus plateau along the eastern edge of Oceanus Procellarum. Although variations in the crustal thickness might act to modulate the amount of magma that ultimately reaches the surface, this hypothesis does not explain why the farside South Pole-Aitken basin, whose crust is thinner than Oceanus Procellarum, was only modestly filled by volcanic products. The ages of the mare basalts have been determined both by direct radiometric dating and by the technique of crater counting. The highlands are older than the visible maria, and hence are more heavily cratered.
On the Moon, surfaces are either densely covered by large craters (lunar highlands) or sparsely affected by large craters (maria) with no surfaces of intermediate crater densities. By using lunar core samples, one could determine a density profile of the soil with depth near the landing sites, as well as the complex dielectric constant of a variety of rocks and powders. (b) A residual map of Mercury, which shows the residuals after subtracting a model image from the observed map. The most distinctive aspect of the Moon is the contrast between its bright and dark zones. The brightness scale in R assumes an average effective area of 100 cm2 for the ROSAT PSPC over the lunar spectrum. In the case of the Moon, a minimum of 6000 craters with diameters greater than 20 km are believed to have been formed during this early period. Red corresponds to higher than average densities and blue corresponds to lower than average densities. Relative concentration of various elements on the lunar surface (in weight %), Relative concentration (in weight %) of various elements on lunar highlands, lunar lowlands, and Earth, Yu.
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