Lunar Report for Astronomy
In the field of astronomy, lunar is a term used to refer to any object related to the moon. Thus, the word lunar is often used interchangeably with the term moon.
General Lunar Background
The term “lunar” is derived from the ancient Greek goddess of the moon called luna (May 37). According to Greek mythology, luna is perceived as the compliment to the god of the sun referred to as Sol. Hence, the moon appears at night while the sun appears during the day.
The moon revolves around the Earth and is the Earth’s only satellite that occurs naturally. Also, it is the fifth-biggest satellite in the Solar system. In comparison to other planetary satellites, the moon is the largest concerning planet size. Jupiter’s satellite is the largest, followed by the moon. Finally, it is the second in terms of density.
Scientists perceive that the moon was formed approximately 4.51 billion years ago, shortly after the Earth was created (Barboni et al. 1). The most logical explanation for its formation is that after a hypothetical object the size of Mars called Theia collided with the Earth, the considerable impact resulted in debris that later became the moon. The impact shattered materials into the Earth’s orbit that coalesced and formed the moon. Astronauts and scientists have widely accepted this theory as giant effects were common during the formation of the solar system. However, new studies have shown that the moon may be slightly older than it is thought.
The moon and the Earth are in synchronous rotation, and as a result, the moon always shows one side to the Earth. However, approximately 59% of the moon is visible from the Earth because of a phenomenon called libration. Libration is the real or apparent rotation of the moon that allows viewing of some of the parts of the lunar surface that are typically invisible. The moon is the brightest celestial object after the sun in Earth’s sky. Despite having a dark surface, it appears bright at night because of its reflection capability that exceeds that of worn asphalt. The moon’s gravitational force is responsible for the slight lengthening of a typical day, body tides, and ocean tides.
The approximate orbital distance of the moon is 384,402 km or 1.28 light-seconds. This distance is about 30 times the Earth’s diameter. Both the sun and the moon appear to be the same size since the former is 400 times the diameter and distance of the latter. Consequently, during the total solar eclipse, the sun is covered by the moon. Nonetheless, this phenomenon is thought to stop in the future since the distance of the Earth and moon is increasing gradually.
Physical Characteristics
As a result of tidal stretching, the moon is a slightly scalene ellipsoid with an axis that is displaced 30° from the Earth. Don't use plagiarised sources.Get your custom essay just from $11/page
Internal Structure
The moon’s inner core is composed of solid iron, while its outer core has liquid iron. A boundary layer of partially molten substance exists around its core as a result of fractional crystallization of magma during formation. Geochemical mapping of the moon’s orbit shows that its crust mostly comprises of anorthosite. The crust is approximately 50km thick.
Lunar Swirls
Lunar swirls are mysterious features across the surface of the moon. They have a sinuous shape and appear to be optically immature due to a high albedo.
Lunar Water
The lunar surface cannot hold liquid water. When the water is exposed to solar radiation, it disappears into space through the process of photodissociation. However, studies in recent years have revealed the existence of small frozen water pockets on the surface of the moon (Deutsch, Head and Neumann 17).
Specifics on Targeted Objects
There are several features related to the moon. Some of these features include Hipparchus, Fracastorius, and Maurolycus.
Hipparchus
Hipparchus is a degraded remnant from a lunar impact crater named after a Greek geographer and astronomer called Hipparchus. This feature is located near the center of the moon, southeast of Sinus Medii. Other features similar to the Hipparchus are Ptolemaeus and Albategnius. Ancient satellite craters share significant features. They have undergone substantial changes in their structures due as a result of subsequent impacts. Hipparchus’s western rim has been eroded and worn away to the point that only low hills are visible on the lunar surface. The Eastern wall is more intact despite the numerous erosion impacts. On the western wall lies two deep clefts that are responsible for two parallel scars in the south-central highlands. The flow of basaltic lava has resurfaced the floor of the crater. However, the southwest part is more rugged and slightly raised s compared to the other sections of the floor. By convention, satellite features are demonstrated on lunar maps by letters placed on the side of the midpoint of the crater. In 1664, a scientist called Robert Hooke used a telescope to view lunar craters and explain their formation (Nakajima 74). He proposed that they resulted from projectile bombardment between subterranean lunar volcanism and space.
Fracastorius
Fracastorius is also an ancient remnant of the lunar impact crater that flooded with lava. It is found in the south of Mare Nectaris. To its northwest is the Beaumont crater, and to its northeast is Rosse. Subsequent impacts have led to the disappearance of its northern wall. Its outline `is only shown by the presence of mounds in the lunar mare. This crater was also invaded by the lava that led to the formation of Mare Nectaris. Thus, Fracastorius forms a bay-like structure. There is little presence of its original rim sue do erosion impacts. The rim’s maximum elevation is approximately 2.4 km. Fractastorius D is the most prominent crater located in the western rim. Fracastorius lacks a central peak. However, it has a long slender rille that runs through the floor’s middle in an east-west direction. These structures are generally represented on lunar maps by letters placed on the side of the midpoint of the Fracastorius crater.
Maurolycus
Maurolycus crater is located on the southern highland side of the lunar surface. Overlapping impacts of lunar craters cover it. The feature was named after an Italian astronomer and mathematician called Francesco Maurolico. It joins a smaller crater called Barocius at the southeast rim. To the west lies an overlapping pair of Faraday and Stofler. Faint craters such as Gemma Frisius and Burch join the Maurolycus crater to the north. Its outer walls are broad, tall, and terraced, especially in the eastern part. The rim is lower and joined to by an overlain rim to the southeast. The Northwest part is more rugged than the rest of the structure. However, other sections are relatively level and have complex peaks and craterlets. Lunar Report for Astronomy
In the field of astronomy, lunar is a term used to refer to any object related to the moon. Thus, the word lunar is often used interchangeably with the term moon.
General Lunar Background
The term “lunar” is derived from the ancient Greek goddess of the moon called luna (May 37). According to Greek mythology, luna is perceived as the compliment to the god of the sun referred to as Sol. Hence, the moon appears at night while the sun appears during the day.
The moon revolves around the Earth and is the Earth’s only satellite that occurs naturally. Also, it is the fifth-biggest satellite in the Solar system. In comparison to other planetary satellites, the moon is the largest in relation to planet size. Jupiter’s satellite is the largest, followed by the moon. Finally, it is the second in terms of density.
Scientists perceive that the moon was formed approximately 4.51 billion years ago, shortly after the Earth was created (Barboni et al. 1). The most logical explanation for its formation is that after a hypothetical object the size of Mars called Theia collided with the Earth, the considerable impact resulted in debris that later became the moon. The impact shattered materials into the Earth’s orbit that coalesced and formed the moon. Astronauts and scientists have widely accepted this theory as giant effects were common during the formation of the solar system. However, new studies have shown that the moon may be slightly older than it is thought.
The moon and the Earth are in synchronous rotation, and as a result, the moon always shows one side to the Earth. However, approximately 59% of the moon is visible from the Earth because of a phenomenon called libration. Libration is the real or apparent rotation of the moon that allows viewing of some of the parts of the lunar surface that are typically invisible. The moon is the brightest celestial object after the sun in Earth’s sky. Despite having a dark surface, it appears bright at night because of its reflection capability that exceeds that of worn asphalt. The moon’s gravitational force is responsible for the slight lengthening of a normal day, body tides, and ocean tides.
The approximate orbital distance of the moon is 384,402 km or 1.28 light-seconds. This distance is about 30 times the Earth’s diameter. Both the sun and the moon appear to be the same size since the former is 400 times the diameter and distance of the latter. Consequently, during the total solar eclipse, the sun is covered by the moon. Nonetheless, this phenomenon is thought to stop in the future since the distance of the Earth and moon is increasing gradually.
Physical Characteristics
As a result of tidal stretching, the moon is a slightly scalene ellipsoid with an axis that is displaced 30° from the Earth.
Internal Structure
The moon’s inner core is composed of solid iron, while its outer core has liquid iron. A boundary layer of partially molten substance exists around its core as a result of fractional crystallization of magma during formation. Geochemical mapping of the moon’s orbit shows that its crust mostly comprises of anorthosite. The crust is approximately 50km thick.
Lunar Swirls
Lunar swirls are mysterious features across the surface of the moon. They have a sinuous shape and appear to be optically immature due to a high albedo.
Lunar Water
The lunar surface cannot hold liquid water. When the water is exposed to solar radiation, it disappears into space through the process of photodissociation. However, studies in recent years have revealed the existence of small frozen water pockets on the surface of the moon (Deutsch, Head and Neumann 17).
Specifics on Targeted Objects
There are several features related to the moon. Some of these features include Hipparchus, Fracastorius, and Maurolycus.
Hipparchus
Hipparchus is a degraded remnant from a lunar impact crater named after a Greek geographer and astronomer called Hipparchus. This feature is located near the center of the moon, southeast of Sinus Medii. Other features similar to the Hipparchus are Ptolemaeus and Albategnius. Ancient satellite craters share significant features. They have undergone substantial changes in their structures due as a result of subsequent impacts. Hipparchus’s western rim has been eroded and worn away to the point that only low hills are visible on the lunar surface. The Eastern wall is more intact despite the numerous erosion impacts. On the western wall lies two deep clefts that are responsible for two parallel scars in the south-central highlands. The flow of basaltic lava has resurfaced the floor of the crater. However, the southwest part is more rugged and slightly raised s compared to the other sections of the floor. By convention, satellite features are demonstrated on lunar maps by letters placed on the side of the midpoint of the crater. In 1664, a scientist called Robert Hooke used a telescope to view lunar craters and explain their formation (Nakajima 74). He proposed that they resulted from projectile bombardment between subterranean lunar volcanism and space.
Fracastorius
Fracastorius is also an ancient remnant of the lunar impact crater that flooded with lava. It is found in the south of Mare Nectaris. To its northwest is the Beaumont crater, and to its northeast is Rosse. Subsequent impacts have led to the disappearance of its northern wall. Its outline is only shown by the presence of mounds in the lunar mare. This crater was also invaded by the lava that led to the formation of Mare Nectaris. Thus, Fracastorius forms a bay-like structure. There is little presence of its original rim sue do erosion impacts. The rim’s maximum elevation is approximately 2.4 km. Fractastorius D is the most prominent crater located in the western rim. Fracastorius lacks a central peak. However, it has a long slender rille that runs through the floor’s middle in an east-west direction. These structures are generally represented on lunar maps by letters placed on the side of the midpoint of the Fracastorius crater.
Maurolycus
Maurolycus crater is located on the southern highland side of the lunar surface. Overlapping impacts of lunar craters cover it. The feature was named after an Italian astronomer and mathematician called Francesco Maurolico. It joins a smaller crater called Barocius at the southeast rim. To the west lies an overlapping pair of Faraday and Stofler. Faint craters such as Gemma Frisius and Burch join the Maurolycus crater to the north. Its outer walls are broad, tall, and terraced, especially in the eastern part. The rim is lower and joined to by an overlain rim to the southeast. The Northwest part is more rugged than the rest of the structure. However, other sections are relatively level and have complex peaks and craterlets.