MAP OF THE MOON, MONDKARTE,HISTORICAL...

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Vintage-Views Antique Prints and Maps :: Antique Prints :: Scientific :: Astronomy :: MAP OF THE MOON, MONDKARTE,HISTORICAL SELENOGRAPHY PRINT,1894 Original Antique Color Engraving

MAP OF THE MOON, MONDKARTE,HISTORICAL SELENOGRAPHY PRINT,1894 Original Antique Color Engraving

The Moon is Earth's only natural satellite. It has no formal English name other than "the Moon", although in English it is occasionally called Luna (Latin for moon), or Selene (Greek for moon), to distinguish it from the generic term "moon" (natural satellites of other planets are also called moons). Its symbol is a crescent. The terms lunar, selene/seleno-, and -cynthion (from the Lunar deities Selene and Cynthia) refer to the Moon (aposelene, selenocentric, pericynthion, etc.). The average distance from the Moon to the Earth is 384,403 kilometres (238,857 mi). The Moon's diameter is 3,476 kilometres (2,160 mi). Reflected sunlight from the Moon's surface reaches Earth in 1.3 seconds (at the speed of light). When observed with earth based telescopes, the moon can be seen to have some 30,000 craters having a diameter of at least 1 km, but close up observation from lunar orbit reveals a multitude of ever smaller craters. Most are hundreds of millions or billions of years old; the lack of atmosphere, weather and recent geological processes ensures that most of them remain permanently preserved. In the lunar terrae, it is indeed impossible to add a crater of any size without obliterating another; this is termed saturation. The largest crater on the Moon, and indeed the largest known crater within the solar system, forms the South Pole-Aitken basin. This crater is located on the far side, near the South Pole, and is some 2,240 kilometres in diameter, and 13 kilometres in depth. The dark and relatively featureless lunar plains are called maria, Latin for seas, since they were believed by ancient astronomers to be water-filled seas. They are actually vast ancient basaltic lava flows that filled the basins of large impact craters. The lighter-colored highlands are called terrae. Maria are found almost exclusively on the Lunar nearside, with the Lunar farside having only a few scattered patches. Blanketed atop the Moon's crust is a dusty outer rock layer called regolith, the result of rocks shattered by billions of years of impacts. Both the crust and regolith are unevenly distributed over the entire Moon. The crust ranges from 60 kilometres (38 mi) thick on the near side to 100 kilometres (63 mi) on the far side, and the regolith varies from 3 to 5 metres (10 to 16 ft) deep in the maria to 10 to 20 metres (33 to 66 ft) deep in the highlands. In 2004, a team led by Dr. Ben Bussey of Johns Hopkins University using images taken by the Clementine mission determined that four mountainous regions on the rim of the 73-km-wide Peary crater at the Moon's north pole appeared to remain illuminated for the entire Lunar day. These unnamed "mountains of eternal light" are possible due to the Moon's extremely small axial tilt, which also gives rise to permanent shadow at the bottoms of many polar craters. No similar regions of eternal light exist at the less mountainous south pole, although the rim of Shackleton crater is illuminated for 80% of the lunar day. Clementine's images were taken during the northern Lunar hemisphere's summer season, and it remains unknown whether these four mountains are shaded at any point during their local winter season. Dating of the lunar impact events through 40Ar/39Ar isotop analysis of glass spherules, created during the impacts, showed a high impact number in early lunar history and in the last 400 million years. MAP HAS AN INDEX ON THE SIDE REFERING TO THE VARIOUS SITES ON THE MAP.

Published for Joseph Meyer Meyers Konversations

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SKU	0527680k6
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Price:	US$50.00

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