Warren Check it out! Global lunar maps shown in a cylindrical projection and truncated at 70° north and south. Thank you for signing up to Space. Both are essential parameters in modeling radio observations of the Moon. The upper layers of the surface are porous, consisting of loosely packed dust into which their boots sank several centimeters (Figure 5). Thousands of individual craters have been named, however, mostly for great scientists and philosophers (Figure 1). 2015), consistent with other FAN ages reported. The ITEs are generally thought to be resistant to impact-shock, and thus may be able to identify the lithology of small clasts/mineral fragments, regardless of the size of the material analysed. For full access to this pdf, sign in to an existing account, or purchase an annual subscription. 2004, Joy 2013, Russell et al. The Moon, like Earth, was formed about 4.5 billion year ago. Note the smooth contours of the lunar mountains, which have not been sculpted by water or ice. These are modeled well, as exemplified by the map in Fig. et al. The lunar Alps, the Montes Alpes, sweep off to the northwest, enclosing the perfect oval crater, Plato. These mesospheric winds likely carry CO, formed on the day side upon photodissociation of CO2, to the night side of the planet. Regular photolysis of water in the martian atmosphere may be too slow, however. Dislocation features within the plagioclase highlight that this sample has undergone shocks. The Moon that we see is dominated by two units with different albedo: the white unit – highlands – which has been scarred by ancient impact events, and the dark unit – lava “mare” flows – that often infills these huge circular basins (figure 2). Note the two so-called hot regions, discussed in the text. et al. 1992, Elkins-Tanton et al. 2012), then the resulting ejecta on the highland crust may mask ferroan signatures from remote-sensing observations, potentially accounting for a range of mineral compositions (MAN and FAN-like fragments) within a single meteorite such as ALHA 81005 (Gross et al. On Earth, mountains are formed by two different processes. In addition to thermal subsidence, the basins may be loaded by later mare volcanism, leading to further subsidence and stress. John F Pernet-Fisher, Katherine H Joy, The lunar highlands: old crust, new ideas, Astronomy & Geophysics, Volume 57, Issue 1, February 2016, Pages 1.26–1.30, https://doi.org/10.1093/astrogeo/atw039. 603–616.). They are made of relatively low-density rock that solidified on the cooling Moon like slag floating on the top of a smelter. 2014, Borg et al. However, this was before the GX5-1 data were acquired, which clearly show lunar night side X-rays from the early morning (trailing) hemisphere as well. The maria are much less cratered than the highlands, and cover just 17% of the lunar surface, mostly on the side of the Moon that faces Earth (Figure 3b). 5 show the night side line to be much deeper and narrower than the day side line, suggestive of a large concentration of CO at high altitudes on the night side of the planet. If such an impact was able to excavate both crustal and Mg-rich mantle material (e.g. Although it is often argued that the sampling from the Apollo missions is dominated by Imbrium ejecta, lunar meteorites have provided fresh insights. Since CO is formed in the upper part of the atmosphere, the line is seen in absorption against the warm continuum background on both Venus and Mars (Fig. 2014), which overlaps ages reported for Mg-suite secondary magmatic rocks (Borg et al. However, reinvestigations of the Apollo collection continues to shed important new light on geological processes, reflecting the fact that there are still many outstanding questions for lunar geoscience. 3b, which shows the difference between the observed map and a thermal model. in the FHT) and polar areas, in comparison to the nearside. Why don't libraries smell like bookstores? Who is the longest reigning WWE Champion of all time? Hurwitz Critically, some of these meteorites are thought to come from the lunar farside (e.g. However, when deeper layers are probed, the diurnal heating pattern is less obvious, and one can distinguish two relatively “hot” regions, one at longitude 0° and one at 180°. There is spectrographs evidence for the Mg-rich mineral pyroxene. They provide samples of lunar crust from highland regions remote from the Apollo landing sites. On Earth there are low viscosity alkali basalts that could produce the type of volcanic morphology represented by Mercury's plains. The FeO content appears to be between 1 and 3%. J., 607, 596–610.] The central mountain rises 12 kilometers above the crater floor. Indeed, when compared with lunar spectral reflectance data from the Clementine spacecraft, the distribution of FeO contents, KREEP-associated U and Th contents, and, indeed, the highlands nature of lunar meteorites themselves parallel the overall lunar character. (c) Observed and background-subtracted spectra from the September 2001 Chandra observation of the dark side of the Moon, with 29-eV binning. The hot regions have been modeled extremely well, since they do not show up in this residual map.
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