Satelit Bulan Bumi

Kesan hentaman dan gunung berapi

Konsekuensi impak yang dominan diperhatikan di setiap pemandangan bulan. Pada skala terbesar adalah lembangan kuno, yang membentang ratusan kilometer. Contoh yang indah ialah Orientale Basin, atau Mare Orientale, yang dinding gunungnya dapat dilihat dari Bumi berhampiran anggota badan Bulan (pinggir cakera lunar yang jelas) ketika liberasi bulan disukai. Tebing berbilang cincinnya merupakan ciri dari lembangan terbesar; mereka beraksen oleh banjir lava separa daerah rendah di antara cincin. Lembangan Orientale merupakan lembangan berukuran besar termuda di Bulan.

Tidak jelas

Bagaimana Anda Beritahu Perbezaan Antara Gerhana Total, Annular, Solar, dan Lunar?

Yang menghalang siapa.

Nama Orientale muncul dari konvensi pemetaan bulan. Pada zaman pemerhatian teleskopik yang hebat pada abad ke-17 hingga ke-19, gambaran Bulan biasanya menunjukkan arah selatan di bahagian atas kerana teleskop membalikkan gambar. Timur dan barat merujuk ke arah yang ada di langit — yaitu, Bulan bergerak ke arah timur dan anggota badannya yang terdahulu berada di sebelah timur, dan bahagian lembangan yang dapat dilihat dari Bumi disebut Mare Orientale. Untuk tujuan pemetaan koordinat bulan diambil berasal dari pusat muka sisi dekat, di persimpangan khatulistiwa dan meridian yang ditentukan oleh perpustakaan min. Sebuah kawah kecil, Mösting A, dipersetujui sebagai titik rujukan. Dengan Bulan dianggap sebagai dunia, bukan hanya cakera yang bergerak melintasi langit, timur dan barat ditukar. Oleh itu, Orientale, walaupun namanya,terletak di garis bujur bulan barat.

Smaller impact features, ranging in diameter from tens of kilometres to microscopic size, are described by the term crater. The relative ages of lunar craters are indicated by their form and structural features. Young craters have rugged profiles and are surrounded by hummocky blankets of debris, called ejecta, and long light-coloured rays made by expelled material hitting the lunar surface. Older craters have rounded and subdued profiles, the result of continued bombardment.

A crater’s form and structure also yield information about the impact process. When a body strikes a much larger one at speeds of many kilometres per second, the available kinetic energy is enough to completely melt, even partly vaporize, the impacting body along with a small portion of its target material. On impact, a melt sheet is thrown out, along with quantities of rubble, to form the ejecta blanket around the contact site. Meanwhile, a shock travels into the subsurface, shattering mineral structures and leaving a telltale signature in the rocks. The initial cup-shaped cavity is unstable and, depending on its size, evolves in different ways. A typical end result is the great crater Aristarchus, with slumping terraces in its walls and a central peak. Aristarchus is about 40 km (25 miles) in diameter and 4 km (2.5 miles) deep.

The region around Aristarchus shows a number of peculiar lunar features, some of which have origins not yet well explained. The Aristarchus impact occurred on an elevated, old-looking surface surrounded by lavas of the northern part of the mare known as Oceanus Procellarum. These lava flows inundated the older crater Prinz, whose rim is now only partly visible. At one point on the rim, an apparently volcanic event produced a crater; subsequently, a long, winding channel, called a sinuous rille, emerged to flow across the mare. Other sinuous rilles are found nearby, including the largest one on the Moon, discovered by the German astronomer Johann Schröter in 1787. Named in his honour, Schröter’s Valley is a deep, winding channel, hundreds of kilometres long, with a smaller inner channel that meanders just as slow rivers do on Earth. The end of this “river” simply tapers away to nothing and disappears on the mare plains. In some way that remains to be accounted for, hundreds of cubic kilometres of fluid and excavated mare material vanished.

The results of seismic and heat-flow measurements suggest that any volcanic activity that persists on the Moon is slight by comparison with that of Earth. Over the years reliable observers have reported seeing transient events of a possibly volcanic nature, and some spectroscopic evidence for them exists. In the late 1980s a cloud of sodium and potassium atoms was observed around the Moon, but it was not necessarily the result of volcanic emissions. It is possible that interactions of the lunar surface and the solar wind produced the cloud. In any case, the question of whether the Moon is volcanically active remains open.

Telescopic observers beginning in the 19th century applied the term rille to several types of trenchlike lunar features. In addition to sinuous rilles, there are straight and branching rilles that appear to be tension cracks, and some of these—such as Rima Hyginus and the rilles around the floor of the large old crater Alphonsus—are peppered with rimless eruption craters. Though the Moon shows both tension and compression features (low wrinkle ridges, usually near mare margins, may result from compression), it gives no evidence of having experienced the large, lateral motions of plate tectonics marked by faults in Earth’s crust.

Among the most enigmatic features of the lunar surface are several light, swirling patterns with no associated topography. A prime example is Reiner Gamma, located in the southeastern portion of Oceanus Procellarum. Whereas other relatively bright features exist—e.g., crater rays—they are explained as consequences of the impact process. Features such as Reiner Gamma have no clear explanation. Some scientists have suggested that they are the marks of comet impacts, in which the impacting body was large in size but had so little density as to produce no crater. Reiner Gamma is also unusual in that it coincides with a large magnetic anomaly (region of magnetic irregularity) in the crust.

Small-scale features

On a small-to-microscopic scale, the properties of the lunar surface are governed by a combination of phenomena—impact effects due to the arrival, at speeds up to tens of kilometres per second, of meteoritic material ranging in size down to fractions of a micrometre; bombardment by solar-wind, cosmic-ray, and solar-flare particles; ionizing radiation; and temperature extremes. Subject to no meteorological effects and unprotected by a substantial atmosphere, the uppermost surface reaches almost 400 kelvins (K; 260 °F, 127 °C) during the day and plunges to below 100 K (−279 °F, −173 °C) at night. The top layer of regolith, however, serves as an efficient insulator because of its high porosity (large number of voids, or pore spaces, per unit of volume). As a result, the daily temperature swings penetrate into the soil to less than one metre (about three feet).

Long before human beings could observe the regolith firsthand, Earth-based astronomers concluded from several kinds of measurements that the Moon’s surface must be very peculiar. The evidence from photometry (brightness measurements) is particularly striking. From Earth the fully illuminated Moon is 11 times as bright as one only half illuminated, and it appears bright up to the edge of the disk. Measurements of the amount of sunlight reflected back in the direction of illumination indicate the reason: on a small scale the surface is extremely rough, and light reflected from within mineral grains and deep cavities remains shadowed until the illumination source is directly behind the observer—i.e., until the full moon—at which time light abruptly reflects out of the cavities. The polarization properties of the reflected light show that the surface is rough even at a microscopic scale.

Before spacecraft landed on the Moon, astronomers had no straightforward means by which to measure the depth of the regolith layer. Nevertheless, after the development of infrared detectors allowed them to make accurate thermal observations through the telescope, they could finally draw some reasonable conclusions about the outer surface characteristics. As Earth’s shadow falls across the Moon during a lunar eclipse, the lunar surface cools rapidly, but the cooling is uneven, being slower near relatively young craters where exposed rock fields are to be expected. This behaviour could be interpreted to show that the highly insulating layer is fairly shallow, a few metres at most. Though not all astronomers accepted this conclusion at first, it was confirmed in the mid-1960s when the first robotic spacecraft soft-landed and sank only a few centimetres instead of disappearing completely into the regolith.