Information about Orbit Of The Moon
The orbit of the Moon around the Earth is completed in approximately 27.3 days. The Earth and Moon orbit about their common center of mass, which lies about 4,700 kilometres from Earth's center (about three quarters of the Earth's radius). On average, the Moon is at a distance of about 385,000 km from the center of the Earth, which corresponds to about 60 Earth radii. With a mean orbital speed of 1.023 km/s, the Moon moves relative to the stars each hour by an amount roughly equal to its angular diameter, or by about 0.5°. The Moon differs from most satellites of other planets in that its orbit is close to the plane of the ecliptic, and not to the Earth's equatorial plane. The lunar orbit plane is inclined to the ecliptic by 5.1°, whereas the Moon's spin axis is inclined by only 1.5°.
The distance between the center of masses of the Earth and Moon is, averaged over time, about 385,000 km, corresponding to about 60 Earth radii or 30 Earth diameters. Both bodies orbit about their common center of mass (the barycenter), which is located at about 4,670 kilometres from the center of the Earth, or 1700 km below the Earth's surface. Because of the relatively large size of the Moon and the relatively small Earth/Moon mass ratio of about 81:1 (when compared to other natural satellites in our solar system), some consider the Earth-Moon system to be a double planet. Based on the informal definition that a double planet system must have its barycentre exterior to both bodies, others, however, regard the Earth and Moon as an ordinary planet-moon system.
The orbit of the Moon is distinctly elliptical with an average eccentricity of 0.0549. The non-circular form of the lunar orbit causes variations in the Moon's angular speed and apparent size as it moves towards and away from an observer on Earth. The mean angular daily movement relative to an imaginary observer at the barycentre is 13.176358° to the east. The orientation of the orbit is not fixed in space, but precesses over time. One motion is the recession of the line of apsides: the ellipse of the lunar orbit slowly rotates counterclockwise, and completes a full revolution in about 8.850 years (3233 days). The other motion is associated with the (clockwise) precession of the orbital plane itself about an axis perpendicular to the ecliptic. The points where the lunar orbit intersects the ecliptic (the nodes) precess with time, completing one revolution in about 18.6 years (6793 days).
The mean inclination of the lunar orbit to the ecliptic plane is 5.145°. The rotation axis of the Moon is also not perpendicular to its orbital plane, so the lunar equator is not in the plane of its orbit, but is inclined to it by a constant value of 6.688° (this is the obliquity). One might be tempted to think that as a result of the precession of the Moon's orbit plane, the angle between the lunar equator and the ecliptic would vary between the sum (11.833°) and difference (1.543°) of these two angles. However, as was discovered by Jacques Cassini in 1721, the rotation axis of the Moon precesses with the same rate as its orbit plane, but is 180° out of phase (see Cassini's Laws). Thus, although the rotation axis of the Moon is not fixed with respect to the stars, the angle between the ecliptic and the lunar equator is always 1.543°.
There are several ways to consider how much time it takes the Moon to complete one orbit. The sidereal month is the time it takes to make one complete orbit with respect to the fixed stars, which is about 27.3 days. In contrast, the synodic month is the time it takes the Moon to reach the same phase, which takes about 29.5 days. The synodic period is longer than the sidereal period because the Earth-Moon system moves a finite distance in its orbit around the Sun during each sidereal month, and a longer time is required to achieve the same relative geometry. Other definitions for the duration of a lunar month include the time it takes to go from perigee to perigee (the anomalistic month), from ascending node to ascending node (the Draconic month), and from two successive passes of the same ecliptic longitude (the Tropical month). As a result of the slow precession of the lunar orbit, these latter three periods are only slightly different than the sidereal month. The average length of a calendric month (1/12 of a year) is about 30.4 days..
The tidal bulges on Earth are carried ahead of the Earth-Moon axis by a small amount as a result of the Earth's rotation. This is a direct consequence of friction and the dissipation of energy as water moves over the ocean bottom and into or out of bays and estuaries. Each bulge exerts a small amount of gravitational attraction on the moon, with the bulge closest to the moon pulling in a direction slightly forward along the moon's orbit, because the earth's rotation has carried the bulge forward. The opposing bulge has the opposite effect, but the closer bulge dominates due to its comparative closer distance to the moon. As a result, some of the Earth's rotational momentum is gradually being transferred to the Moon's orbital momentum, and this causes the Moon to slowly recede from Earth at the rate of approximately 38 millimetres per year. Due to conservation of angular momentum, the Earth's rotation is gradually slowing, and the Earth's day thus lengthens by about 17 microseconds every year (this would make each Earth day one second longer every 60,000 years or so, by one minute longer every four million years, and by four hours longer in 1 billion years' time. Looking back, the day was a mere 23h in length when the Dinosaurs roamed the Earth 65 million years ago). See tidal acceleration for a more detailed description and references.
So the Moon is gradually receding from the Earth into a higher orbit, and calculations (by e.g. NASA at the Jet Propulsion Laboratory [1]) suggest that this will continue for about two billion years. By that time, the Earth and Moon will become caught up in what are called a "spin-orbit resonance" in which the Moon will circle the Earth in about 47 days (currently 29 days) and both Moon and Earth will rotate around their axes in the same time, always facing each other with the same side. Beyond this, it is hard to tell what will happen to the Earth-Moon system.
The Moon is in synchronous rotation, meaning that it keeps the same face turned toward the Earth at all times. This synchronous rotation is only true on average because the Moon's orbit has a definite eccentricity. As a result, the angular velocity of the Moon varies as it moves around the Earth, and is hence not always equal to the Moon's rotational velocity. When the Moon is at its perigee, its rotation is slower than its orbital motion, and this allows us to see up to eight degrees of longitude of its Eastern (right) far side. Conversely, when the Moon reaches its apogee, its rotation is faster than its orbital motion and this reveals eight degrees of longitude of its Western (left) far side. This is referred to a longitudinal libration.
Because the lunar orbit is also inclined to the Earth's ecliptic plane by 5.1° , the rotation axis of the Moon seems to rotate towards and away from us during one complete orbit. This is referred to as a latitudinal libration, which allows one to see almost 7° of latitude beyond the pole on the far side. Finally, because the Moon is only about 60 Earth radii away from the Earth's center of mass, an observer at the equator who observes the Moon throughout the night moves laterally by one Earth diameter. This gives rise to a diurnal libration, which allows one to view an additional one degree's worth of lunar longitude. For the same reason, observers at both geographical poles of the Earth would be able to see one additional degree's worth of libration in latitude.
In representations of the Solar system, it is common to draw the trajectory of the Earth from the point of view of the Sun, and the trajectory of the Moon from the point of view of the Earth. This could give the impression that the trajectory of the Moon circles around the Earth in such a way that sometimes it goes backwards when viewed from the Sun's perspective. Since the orbital velocity of the Moon about the Earth (1 km/s) is small compared to the orbital velocity of the Earth about the Sun (30 km/s), this never occurs.
Unlike most other moons in the Solar System, the annual trajectory of the Moon is very similar to the one of the Earth. It is always concave towards the Sun, and is nowhere convex or looped.[2][3] Nevertheless, this behaviour should not be taken to mean that the Moon orbits the Sun, and not the Earth. If the gravitational attraction of our Sun could be "turned off," the Moon would continue to make one orbit about the Earth with its current sidereal period. If the Earth-Moon system could be transported to the far reaches of our solar system where the orbital velocity was less than 1 km/s, then the Moon would indeed sometimes move backwards from the vantage point of non-rotating coordinate system centered at the Sun.
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Inclination in general is the angle between a reference plane and another plane or axis of direction.
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Properties of the lunar orbit
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Definition of orbital parameters.
| Property | Value |
|---|---|
| Semi-major axis | ~384 748 km |
| Distance at perigee | ~364 397 km |
| Distance at apogee | ~406 731 km |
| Mean eccentricity | 0.0549006 (0.044 – 0.067) |
| Mean inclination of orbit to ecliptic | 5.145° |
| Mean obliquity | 6.688° |
| Mean inclination of lunar equator to ecliptic | 1.543° |
| Period of precession of nodes | 18.5996 years |
| Period of recession of line of apsides | 8.8504 years |
The distance between the center of masses of the Earth and Moon is, averaged over time, about 385,000 km, corresponding to about 60 Earth radii or 30 Earth diameters. Both bodies orbit about their common center of mass (the barycenter), which is located at about 4,670 kilometres from the center of the Earth, or 1700 km below the Earth's surface. Because of the relatively large size of the Moon and the relatively small Earth/Moon mass ratio of about 81:1 (when compared to other natural satellites in our solar system), some consider the Earth-Moon system to be a double planet. Based on the informal definition that a double planet system must have its barycentre exterior to both bodies, others, however, regard the Earth and Moon as an ordinary planet-moon system.
The orbit of the Moon is distinctly elliptical with an average eccentricity of 0.0549. The non-circular form of the lunar orbit causes variations in the Moon's angular speed and apparent size as it moves towards and away from an observer on Earth. The mean angular daily movement relative to an imaginary observer at the barycentre is 13.176358° to the east. The orientation of the orbit is not fixed in space, but precesses over time. One motion is the recession of the line of apsides: the ellipse of the lunar orbit slowly rotates counterclockwise, and completes a full revolution in about 8.850 years (3233 days). The other motion is associated with the (clockwise) precession of the orbital plane itself about an axis perpendicular to the ecliptic. The points where the lunar orbit intersects the ecliptic (the nodes) precess with time, completing one revolution in about 18.6 years (6793 days).
The mean inclination of the lunar orbit to the ecliptic plane is 5.145°. The rotation axis of the Moon is also not perpendicular to its orbital plane, so the lunar equator is not in the plane of its orbit, but is inclined to it by a constant value of 6.688° (this is the obliquity). One might be tempted to think that as a result of the precession of the Moon's orbit plane, the angle between the lunar equator and the ecliptic would vary between the sum (11.833°) and difference (1.543°) of these two angles. However, as was discovered by Jacques Cassini in 1721, the rotation axis of the Moon precesses with the same rate as its orbit plane, but is 180° out of phase (see Cassini's Laws). Thus, although the rotation axis of the Moon is not fixed with respect to the stars, the angle between the ecliptic and the lunar equator is always 1.543°.
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The Moon orbiting Earth, sizes and distances to scale.
The lunar month
- See also:
| The Moon's periods | |||||||||||||||||
| Name | Value (d) | Definition |
|---|---|---|
| sidereal | 27.321 661 | With respect to the distant stars (13.369 passes per year) |
| synodic | 29.530 589 | With respect to the Sun (phases of the Moon, 12.369 cycles per year) |
| tropical | 27.321 582 | With respect to the vernal point (precesses in ~26,000 a) |
| anomalistic | 27.554 550 | With respect to the perigee (recesses in 3232.6 d = 8.8504 a) |
| draconic (nodical) | 27.212 221 | With respect to the ascending node (precesses in 6793.5 d = 18.5996 a) |
Tidal evolution of the lunar orbit
- See also: , , and
The tidal bulges on Earth are carried ahead of the Earth-Moon axis by a small amount as a result of the Earth's rotation. This is a direct consequence of friction and the dissipation of energy as water moves over the ocean bottom and into or out of bays and estuaries. Each bulge exerts a small amount of gravitational attraction on the moon, with the bulge closest to the moon pulling in a direction slightly forward along the moon's orbit, because the earth's rotation has carried the bulge forward. The opposing bulge has the opposite effect, but the closer bulge dominates due to its comparative closer distance to the moon. As a result, some of the Earth's rotational momentum is gradually being transferred to the Moon's orbital momentum, and this causes the Moon to slowly recede from Earth at the rate of approximately 38 millimetres per year. Due to conservation of angular momentum, the Earth's rotation is gradually slowing, and the Earth's day thus lengthens by about 17 microseconds every year (this would make each Earth day one second longer every 60,000 years or so, by one minute longer every four million years, and by four hours longer in 1 billion years' time. Looking back, the day was a mere 23h in length when the Dinosaurs roamed the Earth 65 million years ago). See tidal acceleration for a more detailed description and references.
So the Moon is gradually receding from the Earth into a higher orbit, and calculations (by e.g. NASA at the Jet Propulsion Laboratory [1]) suggest that this will continue for about two billion years. By that time, the Earth and Moon will become caught up in what are called a "spin-orbit resonance" in which the Moon will circle the Earth in about 47 days (currently 29 days) and both Moon and Earth will rotate around their axes in the same time, always facing each other with the same side. Beyond this, it is hard to tell what will happen to the Earth-Moon system.
Libration
)
Animation of the Moon as it cycles through its phases. The apparent wobbling of the Moon is known as libration.
Because the lunar orbit is also inclined to the Earth's ecliptic plane by 5.1° , the rotation axis of the Moon seems to rotate towards and away from us during one complete orbit. This is referred to as a latitudinal libration, which allows one to see almost 7° of latitude beyond the pole on the far side. Finally, because the Moon is only about 60 Earth radii away from the Earth's center of mass, an observer at the equator who observes the Moon throughout the night moves laterally by one Earth diameter. This gives rise to a diurnal libration, which allows one to view an additional one degree's worth of lunar longitude. For the same reason, observers at both geographical poles of the Earth would be able to see one additional degree's worth of libration in latitude.
The Earth & Moon's path around the Sun
)
)
The Earth & Moon's path around the Sun is always concave to the Sun (far left down)
Unlike most other moons in the Solar System, the annual trajectory of the Moon is very similar to the one of the Earth. It is always concave towards the Sun, and is nowhere convex or looped.[2][3] Nevertheless, this behaviour should not be taken to mean that the Moon orbits the Sun, and not the Earth. If the gravitational attraction of our Sun could be "turned off," the Moon would continue to make one orbit about the Earth with its current sidereal period. If the Earth-Moon system could be transported to the far reaches of our solar system where the orbital velocity was less than 1 km/s, then the Moon would indeed sometimes move backwards from the vantage point of non-rotating coordinate system centered at the Sun.
See also
- Ernest William Brown
- Lunar phase
- Orbital elements
- Precession
- List of orbits
- Axial tilt
- Milankovitch cycles
- Astrological age
- Great year
- Orbital eccentricity
- Equinox
References
1. ^ Dickinson, Terence (1993). From the Big Bang to Planet X. Camden East, Ontario: Camden House, 79-81. ISBN 0-921820-71-2.
2. ^ The Orbit of the Moon around the Sun is Convex!. Retrieved on 2006-04-21.
3. ^ Vacher, H.L. (Nov 2001). "Computational Geology 18 - Definition and the Concept of Set" (PDF). Journal of Geoscience Education (5): 470-479. Retrieved on 2006-04-21.
2. ^ The Orbit of the Moon around the Sun is Convex!. Retrieved on 2006-04-21.
3. ^ Vacher, H.L. (Nov 2001). "Computational Geology 18 - Definition and the Concept of Set" (PDF). Journal of Geoscience Education (5): 470-479. Retrieved on 2006-04-21.
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) Moon
The Moon as seen by an observer on Earth
Orbital characteristics
Periapsis: 363,104 km
0.0024 AU
Apoapsis: 405,696 km
0.0027 AU
Semi-major axis: 384,399 km
0.
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The Moon as seen by an observer on Earth
Orbital characteristics
Periapsis: 363,104 km
0.0024 AU
Apoapsis: 405,696 km
0.0027 AU
Semi-major axis: 384,399 km
0.
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EARTH was a short-lived Japanese vocal trio which released 6 singles and 1 album between 2000 and 2001. Their greatest hit, their debut single "time after time", peaked at #13 in the Oricon singles chart.
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STARS can mean:
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- Shock Trauma Air Rescue Society
- Special Tactics And Rescue Service, a fictional task force that appears in Capcom's Resident Evil video game franchise.
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The angular diameter of an object as seen from a given position is the diameter measured as an angle. It can be calculated using the formula:
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- ,
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satellite is an object which has been placed into orbit by human endeavor. Such objects are sometimes called artificial satellites to distinguish them from natural satellites such as the Moon.
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planet, as defined by the International Astronomical Union (IAU), is a celestial body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, not massive enough to cause thermonuclear fusion in its core, and has cleared its neighbouring region of
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ecliptic is the apparent path that the Sun traces out in the sky, as it appears to move in the sky in relation to the stars, this apparent path aligns with the planets throughout the course of the year.
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celestial sphere is an imaginary rotating sphere of "gigantic radius", concentric and coaxial with the Earth. All objects in the sky can be thought of as lying upon the sphere.
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This article is about rotation as a movement of a physical body. For other uses, see Rotation (disambiguation).
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semi-major axis (also semimajor axis) is used to describe the dimensions of ellipses and hyperbolae.
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Ellipse
The major axis of an ellipse is its longest diameter, a line that runs through the centre and both foci, its ends being at the widest points of the shape...... Click the link for more information.
orbit's eccentricity, is an important parameter of the orbit that defines its absolute shape. Eccentricity may be interpreted as a measure of how much this shape deviates from a circle.
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For the science fiction novella by William Shunn, see .
Inclination in general is the angle between a reference plane and another plane or axis of direction.
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In astronomy, axial tilt is the inclination angle of a planet's rotational axis in relation to a perpendicular to its orbital plane. It is also called axial inclination or obliquity.
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nodal period is about twice as long as the apsidal precession period discussed above. After the nodal period, the number of draconic months counted exceed the number of sidereal months counted by exactly one: this happens after about 6793 days (18.6 years).
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center of mass of a system of particles is a specific point at which, for many purposes, the system's mass behaves as if it were concentrated. The center of mass is a function only of the positions and masses of the particles that comprise the system.
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A natural satellite is an object that orbits a planet or other body larger than itself and which is not man-made. Such objects are often called moons. Technically, the term could also refer to a planet orbiting a star, or even to a star orbiting a galactic center, but these
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double planet is an informal term used to describe two planets that orbit each other about a common center of mass that is not located within the interior of either planet: The formal term is "binary system".
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orbit's eccentricity, is an important parameter of the orbit that defines its absolute shape. Eccentricity may be interpreted as a measure of how much this shape deviates from a circle.
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nodal period is about twice as long as the apsidal precession period discussed above. After the nodal period, the number of draconic months counted exceed the number of sidereal months counted by exactly one: this happens after about 6793 days (18.6 years).
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In astrodynamics apse line (or line of apsides) is a common name for an imaginary line defined by orbit's eccentricity vector. It is strictly defined for elliptic, parabolic, and hyperbolic orbits.
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perpendicular (or orthogonal) to each other if they form congruent adjacent angles. The term may be used as a noun or adjective. Thus, referring to Figure 1, the line AB is the perpendicular to CD through the point B.
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ecliptic is the apparent path that the Sun traces out in the sky, as it appears to move in the sky in relation to the stars, this apparent path aligns with the planets throughout the course of the year.
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lunar nodes are the orbital nodes of the Moon, that is, the points where the orbit of the Moon crosses the ecliptic (which is the apparent path of the Sun across the heavens against the background stars).
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In astronomy, axial tilt is the inclination angle of a planet's rotational axis in relation to a perpendicular to its orbital plane. It is also called axial inclination or obliquity.
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Jacques Cassini (February 8, 1677 - April 18, 1756) was a French-Italian astronomer, son of the famous Italian astronomer Giovanni Domenico Cassini.
Cassini was born at the Paris Observatory.
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Cassini was born at the Paris Observatory.
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Cassini's Laws (1693) deal with the motion of the Moon.
The first law states that the Moon has 1:1 orbital resonance. This means that the rotation / orbit of the Moon is such that the same face is always facing the Earth.
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The first law states that the Moon has 1:1 orbital resonance. This means that the rotation / orbit of the Moon is such that the same face is always facing the Earth.
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A year (from Old English gēr) is the time between two recurrences of an event related to the orbit of the Earth around the Sun. By extension, this can be applied to any planet: for example, a "Martian year" is the time in which Mars completes its own orbit.
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equinox can have two meanings:
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- The moment when the Sun is positioned directly over the Earth's equator and, by extension, the apparent position of the Sun at that moment - see below.
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Lunar phase refers to the appearance of the illuminated portion of the Moon as seen by an observer, usually on Earth. The lunar phases vary cyclically as the Moon orbits the Earth, according to the changing geometry of the Earth, Moon, and Sun.
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The Sun
Observation data
Mean distance
from Earth 1.4961011 m
(8.31 min at light speed)
Visual brightness (V) −26.74m [1]
Absolute magnitude 4.
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Observation data
Mean distance
from Earth 1.4961011 m
(8.31 min at light speed)
Visual brightness (V) −26.74m [1]
Absolute magnitude 4.
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