Through Every Dark Night There's A Brighter Day Tattoo

Through Every Dark Night There's A Brighter Day Tattoo – “Dark Side of the Moon” rebroadcast here. For the Pink Floyd album, see The Dark Side of the Moon. For other uses, see Dark Side of the Moon (disambiguation).

Photograph of the far side of the Moon, showing Mare Oritale (middle left) and the center of Apollo Crater (top left), taken by the Orion spacecraft during the Artemis 1 mission

Through Every Dark Night There's A Brighter Day Tattoo

The far side of the Moon is the lunar hemisphere that is always facing away from Earth, across to the near side, due to the synchronous rotation in the Moon’s orbit. Compared to the far side, the terrain on the far side is rugged, with many impact craters and relatively few flat and dark lunar maria (“seas”), giving it an appearance closer to other barren places in the Solar System. Mercury and Callisto. It has one of the largest craters in the solar system, the South Port-Aitk basin. The hemisphere is sometimes called the “dark side of the moon,” where “dark” means “unknown” instead of “lack of sunlight”—each side of the moon gets two weeks of sunlight while the other side acclimates. two weeks at night.

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About 18 percent of the far side is occasionally visible from Earth due to libration. The remaining 82 percts were not observed until 1959, when they were photographed by the Soviet space probe Luna 3. The first Far Side atlas was published by the Soviet Academy of Sciences in 1960. The Apollo 8 astronauts were the first to see the Far Side in person when they orbited the Moon in 1968. Each soft landing has been on the manned and unmanned Moon until January 3, 2019, when the Chang’e 4 probe landed on the far side for the first time.

Astronomers proposed installing a large radio telescope on the far side, where the Moon would shield it from possible radio interference from Earth.

Due to tidal locking, residents of the central body (Earth) will never be able to see the wide area of ​​the satellite (Moon).

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Tidal forces from Earth have slowed the Moon’s rotation to the point that the same side always faces Earth—a phenomenon known as tidal locking. Therefore, the other side, most of which is never visible from Earth, is called the “far side of the Moon”. Over time, some of the crescent-shaped edges on the other side may be due to libration.

In total, 59 percent of the Moon’s surface is visible from Earth at one time or another. The parts of the far side of the Moon that are occasionally visible from Earth are difficult to usefully observe because of the low viewing angle from Earth (they cannot be seen “in full”).

A common misconception is that the Moon does not rotate on its axis. If this were the case, the entire Moon would be visible to Earth during its orbit. Instead, its rotation period coincides with its orbital period, meaning it turns once for every orbit it completes: in Earth terms, its day and year could be said to have the same declination (ie ~29.5 clay days ).

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The phrase “dark side of the moon” refers not to “darkness” as in the absence of light, but to “darkness” as in the unknown: until humans were able to send spacecraft around the moon, this region never existed.

In fact, both sides and the far side (on average) receive almost the same amount of direct light from the Sun. This symmetry is complicated by sunlight reflected from Earth to the near side (earth light),

And during a lunar eclipse, which occurs only when the far side is already dark. A lunar eclipse means that the side facing the Earth receives a smaller fraction of sunlight for a long period of time than the side away from it.

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On a “full moon” night, 10 lux of illumination falls on the near side of the moon (about what city sidewalks receive under streetlights; that’s 34 times more light than on Earth during a full moon), but not on the far side. The moon during a lunar night is only about 0.001 lux of starlight.

During a full moon (as seen from Earth), the far side of the Moon is completely dark.

The word dark has also extended to mean that communications with the spacecraft may be blocked when the spacecraft is on the far side of the Moon, such as during the Apollo space missions.

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The two hemispheres of the Moon look different, with the adjacent side covered by a large, multiple maria (Latin for “sea”, since the earliest astronomers mistakenly believed that these plains were seas of lunar water). It looks battered, scratched on the other side and there is a little Maria. Only 1% of the surface of the reverse side is covered by Maria,

Compared to 31.2% on the near side. One commonly accepted explanation for this difference is related to the higher concentration of heat-producing elements in the near-side hemisphere, as shown by geochemical maps obtained from the Lunar Prospector gamma-ray spectrometer. While other factors such as surface elevation and crustal thickness may affect where the basalt crops out, they do not explain why the South Pole–Aitk basin (which has the lowest elevation on the Moon) also did not have a thin crust. volcanically active as Oceanus Procellarum on the near side.

It has also been suggested that the differences between the two hemispheres could be the result of a collision with a smaller companion moon that also formed as a result of the Theia collision.

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In this model, the impact resulted in an accretion mound rather than a crater, which deposited a hemispherical layer of extt and a thickness possibly proportional to the dimensions of the flanking highlands. However, the chemical composition of the distal end is inconsistent with this model.

On the far side, the crater is more visible. This was thought to be the result of the effects of the moon’s lava flows covering and obscuring the craters, rather than a shielding effect from Earth. NASA has calculated that the Earth occupies only about 4 squares of the 41,000 square degrees of sky as from the Moon. “Because of this, the Earth is negligible as a shield for the Moon [and] both sides of the Moon probably experienced the same number of impacts, but fewer craters are visible on the near side than on the far side due to the outpouring of lava. although both sides gained an equal amount of influence.”

More recent research suggests that heat from Earth at the time of the Moon’s formation is why there are fewer impact craters on the near side. The Moon’s crust consists mainly of plagioclase formed by aluminum and calcium condensed and combined with silicates in the mantle. Soon on the colder side these elements consolidated and therefore had a thicker crust; Sometimes a meteoroid impact on the adjacent side of the thinner crust here would release the basaltic lava that formed the maria, but rarely on the far side.

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An October 7, 1959 image from Luna 3 that showed the far side of the Moon for the first time. Clearly visible is Mare Moscovise (top right) and the central trio of Mare Crisium, Mare Marginis and Mare Smythii (centre left).

When the first-ever image of the far side of the Moon (A) is restored using advanced noise removal techniques (B) and compared to the later NASA LRO mission (C), key features are seen clearly and distinctly face-to-face. visible feature mapping is observed.

Until the late 1950s, little was known about the far side of the Moon. Regularly limited views were allowed of features near the far side of the lunar margin, but only up to 59% of the total lunar surface.

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However, these features were from a low angle, making useful observations impossible (it was difficult to distinguish between a crater and a mountain range). The remaining 82% of the surface, on the other hand, remained unknown and its properties were the subject of much speculation.

An example of a distant feature that can be seen through the library is the Mare Oritale, which is a significant basin of influence nearly 1,000 km (600 mi) long, but was not named as a feature until 1906 by Julius Franz. in Der Mond. The true nature of the basin was discovered in the 1960s when corrected images were projected onto the globe. Lunar Orbiter 4 took a close-up photo of the basin in 1967.

Before space exploration began, astronomers did not expect the side to be significantly different from the side visible to Earth.

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In October 1959, the Soviet probe Luna 3 took the first photographs of the far side of the Moon, eight of which were distinguishable.

The images were analyzed and the Academy of Sciences of the USSR published the first atlas of the far side of the Moon on November 6, 1960.

Containing invisible lunar elements from Earth released in the USSR, introduced

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