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The Lagrangian points (pronounced /ləˈɡreɪndʒiən/; also Lagrange point, Lpoint, or libration point), are the five positions in an orbital configuration where a small object affected only by gravity can theoretically be stationary relative to two larger objects (such as a satellite with respect to the Earth and Moon). The Lagrange points mark positions where the combined gravitational pull of the two large masses provides precisely the centripetal force required to rotate with them. They are analogous to geostationary orbits in that they allow an object to be in a "fixed" position in space rather than an orbit in which its relative position changes continuously. A more precise but technical definition is that the Lagrangian points are the stationary solutions of the circular restricted threebody problem. For example, given two massive bodies in circular orbits around their common center of mass, there are five positions in space where a third body, of comparatively negligible mass, could be placed which would then maintain its position relative to the two massive bodies. As seen in a rotating reference frame with the same period as the two coorbiting bodies, the gravitational fields of two massive bodies combined with the centrifugal force are in balance at the Lagrangian points, allowing the third body to be stationary with respect to the first two bodies. History and conceptsThe three collinear Lagrange points were first discovered by Euler around 1750. In 1772, the ItalianFrench mathematician JosephLouis Lagrange was working on the famous threebody problem when he discovered an interesting quirk in the results. Originally, he had set out to discover a way to easily calculate the gravitational interaction between arbitrary numbers of bodies in a system, because Newtonian mechanics concludes that such a system results in the bodies orbiting chaotically until there is a collision, or a body is thrown out of the system so that equilibrium can be achieved. The logic behind this conclusion is that a system with one body is trivial, as it is merely static relative to itself; a system with two bodies is very simple to solve for, as the bodies orbit around their common center of mass. However, once more than two bodies are introduced, the mathematical calculations become very complicated. A situation arises where you would have to calculate every gravitational interaction between every pair of objects at every point along its trajectory. Lagrange, however, wanted to make this simpler. He did so with a simple hypothesis: The trajectory of an object is determined by finding a path that minimizes the action over time. This is found by subtracting the potential energy from the kinetic energy. With this way of thinking, Lagrange reformulated the classical Newtonian mechanics to give rise to Lagrangian mechanics. With his new system of calculations, Lagrange’s work led him to hypothesize how a third body of negligible mass would orbit around two larger bodies which were already in a nearcircular orbit. In a frame of reference that rotates with the larger bodies, he found five specific fixed points where the third body experiences zero net force as it follows the circular orbit of its host bodies (planets). These points were named “Lagrangian points” in Lagrange's honor. It took over a hundred years before his mathematical theory was observed with the discovery of the Trojan asteroids in the 1900s at the Lagrange points of the Sun–Jupiter system. In the more general case of elliptical orbits, there are no longer stationary points in the same sense: it becomes more of a Lagrangian “area”. The Lagrangian points constructed at each point in time, as in the circular case, form stationary elliptical orbits which are similar to the orbits of the massive bodies. This is due to Newton's second law (), where p = mv (p the momentum, m the mass, and v the velocity) is invariant if force and position are scaled by the same factor. A body at a Lagrangian point orbits with the same period as the two massive bodies in the circular case, implying that it has the same ratio of gravitational force to radial distance as they do. This fact is independent of the circularity of the orbits, and it implies that the elliptical orbits traced by the Lagrangian points are solutions of the equation of motion of the third body. The Lagrangian pointsThe five Lagrangian points are labeled and defined as follows: L_{1}The L_{1} point lies on the line defined by the two large masses M_{1} and M_{2}, and between them. It is the most intuitively understood of the Lagrangian points: the one where the gravitational attraction of M_{2} partially cancels M_{1} gravitational attraction.
The Sun–Earth L_{1} is ideal for making observations of the Sun. Objects here are never shadowed by the Earth or the Moon. The Solar and Heliospheric Observatory (SOHO) is stationed in a Halo orbit at L_{1}, and the Advanced Composition Explorer (ACE) is in a Lissajous orbit, also at the L_{1} point. The Earth–Moon L_{1} allows easy access to lunar and earth orbits with minimal change in velocity and would be ideal for a halfway manned space station intended to help transport cargo and personnel to the Moon and back. L_{2}
The L_{2} point lies on the line defined by the two large masses, beyond the smaller of the two. Here, the gravitational forces of the two large masses balance the centrifugal force on the smaller mass.
The Sun–Earth L_{2} is a good spot for spacebased observatories. Because an object around L_{2} will maintain the same orientation with respect to the Sun and Earth, shielding and calibration are much simpler. It is, however, slightly beyond the reach of Earth's umbra, so solar radiation is not completely blocked. The Wilkinson Microwave Anisotropy Probe is already in orbit around the Sun–Earth L_{2}. The Planck satellite, Herschel Space Observatory, Gaia probe, and James Webb Space Telescope will be placed at the Sun–Earth L_{2}. Earth–Moon L_{2} would be a good location for a communications satellite covering the Moon's far side. If the mass of the smaller object (M_{2}) is much smaller than the mass of the larger object (M_{1}) then L_{1} and L_{2} are at approximately equal distances r from the smaller object, equal to the radius of the Hill sphere, given by: where R is the distance between the two bodies. This distance can be described as being such that the orbital period, corresponding to a circular orbit with this distance as radius around M_{2} in the absence of M_{1}, is that of M_{2} around M_{1}, divided by . Examples: L_{3}The L_{3} point lies on the line defined by the two large masses, beyond the larger of the two.
The Sun–Earth L_{3} point was a popular place to put a "CounterEarth" in pulp science fiction and comic books — though of course, once space based observation was possible via satellites and probes, it was shown to hold no such object. Actually, the Sun–Earth L_{3} is highly unstable, because the gravitational forces of the other planets outweigh that of the Earth (Venus, for example, comes within 0.3 AU of L_{3} every 20 months). L_{4} and L_{5}The L_{4} and L_{5} points lie at the third corners of the two equilateral triangles in the plane of orbit whose common base is the line between the centers of the two masses, such that the point lies behind (L_{5}) or ahead of (L_{4}) the smaller mass with regard to its orbit around the larger mass. The reason these points are in balance is that, at L_{4} and L_{5}, the distances to the two masses are equal. Accordingly, the gravitational forces from the two massive bodies are in the same ratio as the masses of the two bodies, and so the resultant force acts through the barycenter of the system; additionally, the geometry of the triangle ensures that the resultant acceleration is to the distance from the barycenter in the same ratio as for the two massive bodies. The barycenter being both the center of mass and center of rotation of the system, this resultant force is exactly that required to keep a body at the Lagrange point in orbital equilibrium with the rest of the system. (Indeed, the third body need not have negligible mass; the general triangular configuration was discovered by Lagrange in work on the 3body problem.) L_{4} and L_{5} are sometimes called triangular Lagrange points or Trojan points. The name Trojan points comes from the Trojan asteroids at the Sun–Jupiter L_{4} and L_{5} points, which themselves are named after characters from Homer's Iliad (the legendary siege of Troy). Asteroids at the L_{4} point, which leads Jupiter, are referred to as the 'Greek camp', while at the L_{5} point they are referred to as the 'Trojan camp'. These asteroids are (largely) named after characters from the respective sides of the Trojan War.
StabilityThe first three Lagrangian points are technically stable only in the plane perpendicular to the line between the two bodies. This can be seen most easily by considering the L_{1} point. A test mass displaced perpendicularly from the central line would feel a force pulling it back towards the equilibrium point. This is because the lateral components of the two masses' gravity would add to produce this force, whereas the components along the axis between them would balance out. However, if an object located at the L_{1} point drifted closer to one of the masses, the gravitational attraction it felt from that mass would be greater, and it would be pulled closer. (The pattern is very similar to that of tidal forces.) Although the L_{1}, L_{2}, and L_{3} points are nominally unstable, it turns out that it is possible to find stable periodic orbits around these points, at least in the restricted threebody problem. These perfectly periodic orbits, referred to as "halo" orbits, do not exist in a full nbody dynamical system such as the solar system. However, quasiperiodic (i.e. bounded but not precisely repeating) orbits following Lissajous curve trajectories do exist in the nbody system. These quasiperiodic Lissajous orbits are what all Lagrangian point missions to date have used. Although they are not perfectly stable, a relatively modest effort at station keeping can allow a spacecraft to stay in a desired Lissajous orbit for an extended period of time. It also turns out that, at least in the case of Sun–Earth L_{1} missions, it is actually preferable to place the spacecraft in a large amplitude (100,000–200,000 km) Lissajous orbit, instead of having it sit at the Lagrangian point, because this keeps the spacecraft off the direct Sun–Earth line, thereby reducing the impact of solar interference on the Earth–spacecraft communications links. Another interesting and useful property of the collinear Lagrangian points and their associated Lissajous orbits is that they serve as "gateways" to control the chaotic trajectories of the Interplanetary Transport Network. In contrast to the collinear Lagrangian points, the triangular points (L_{4} and L_{5}) are stable equilibria (cf. attractor), provided that the ratio of M_{1}/M_{2} is greater than 24.96. This is the case for the Sun–Earth and, by a smaller margin, the Earth–Moon systems. When a body at these points is perturbed, it moves away from the point, but the Coriolis effect bends the object's path into a stable, kidney bean‐shaped orbit around the point (as seen in the rotating frame of reference). However, in the Earth–Moon case, the problem of stability is greatly complicated by the appreciable solar gravitational influence. Intuitive explanationThis section nonmathematically (intuitively) explains the five Lagrangian points using the Earth–Moon system. Lagrangian points L_{2} through L_{5} only exist in rotating systems, as in the monthly orbiting of the Moon about the Earth. At these points, an outward (fictitious, as explained below) centrifugal force is balanced by the attractive gravitational forces of the Moon and Earth. Imagine a person using his hand to spin a stone at the end of a string. The string provides a tension force that continuously accelerates the stone towards the center. To an ant standing on the stone, however, it seems as if there is a force trying to fling him directly outward from the center. This apparent or fictitious force is called the centrifugal force. This same effect is present in the Earth–Moon system, where the role of the string is played by the summed (or net) effect of the two attractive gravities, and the stone is an asteroid or a spacecraft. The Earth–Moon system rotates about its combined center of mass, or barycenter. Because the Earth is much heavier than the Moon, this point is located within the Earth (about 1700 km below the surface). Any object gravitationally held by the rotating Earth–Moon system will sense a centrifugal force directed away from the barycenter, in the same way as does the ant on the stone. Unlike the other Lagrangian points, L_{1} would exist even in a nonrotating (static or inertial) system. Rotation slightly pushes L_{1} away from the (lighter) Moon towards the (heavier) Earth. L_{1} is slightly unstable (see stability above) because drifting towards the Moon or Earth increases one gravitational attraction while decreasing the other, causing more drift. At Lagrangian points L_{2}, L_{3}, L_{4}, and L_{5}, a satellite feels an outward centrifugal force, away from the barycenter, that exactly balances the attractive gravity of the Earth and Moon. L_{2} and L_{3} are slightly unstable because small changes in satellite position more strongly affect gravity than the balancing centrifugal force. Stability at L_{4} and L_{5} depends crucially on the satellite being pulled in three different directions, namely the outward centrifugal force away from the barycenter, balancing the inward gravitational forces towards the Moon and Earth. The easiest way to understand the stability is that L_{1}, and L_{2}, and L_{3} positions are stable, but stable like a ball balanced on a pin. A soft breeze will toss it out of equilibrium. But the L_{4}, and L_{5} positions are stable more like a ball at the bottom of a bowl. Small perturbations will move it out of place, but it will drift back to the bottom. Lagrangian point missionsThe Lagrangian point orbits have unique characteristics that have made them a good choice for performing some kinds of missions. These missions generally orbit the points rather than occupy them directly. Past and present missions
Future and proposed missions
Natural examplesIn the Sun–Jupiter system several thousand asteroids, collectively referred to as Trojan asteroids, are in orbits around the Sun–Jupiter L_{4} and L_{5} points. Recent observations suggest that the Sun–Neptune L_{4} and L_{5} points, known as the Neptune Trojans, may be very thickly populated, containing large bodies an order of magnitude more numerous than the Jupiter Trojans. Other bodies can be found in the Sun–Mars and Saturn–Saturnian satellite systems. There are no known large bodies in the Sun–Earth system's Trojan points, but clouds of dust surrounding the L_{4} and L_{5} points were discovered in the 1950s. Clouds of dust, called Kordylewski clouds, even fainter than the notoriously weak gegenschein, may also be present in the L_{4} and L_{5} of the Earth–Moon system. The Saturnian moon Tethys has two smaller moons in its L_{4} and L_{5} points, Telesto and Calypso. The Saturnian moon Dione also has two Lagrangian coorbitals, Helene at its L_{4} point and Polydeuces at L_{5}. The moons wander azimuthally about the Lagrangian points, with Polydeuces describing the largest deviations, moving up to 32 degrees away from the Saturn–Dione L_{5} point. Tethys and Dione are hundreds of times more massive than their "escorts" (see the moons' articles for exact diameter figures; masses are not known in several cases), and Saturn is far more massive still, which makes the overall system stable. Other coorbitalsThe Earth's companion object 3753 Cruithne is in a relationship with the Earth which is somewhat Trojanlike, but different from a true Trojan. This asteroid occupies one of two regular solar orbits, one of them slightly smaller and faster than the Earth's orbit, and the other slightly larger and slower. The asteroid periodically alternates between these two orbits due to close encounters with Earth. When the asteroid is in the smaller, faster orbit and approaches the Earth, it gains orbital energy from the Earth and moves up into the larger, slower orbit. It then falls farther and farther behind the Earth, and eventually Earth approaches it from the other direction. Then the asteroid gives up orbital energy to the Earth, and drops back into the smaller orbit, thus beginning the cycle anew. The cycle has no noticeable impact on the length of the year, because Earth's mass is over 20 billion (2 × 10) times more than 3753 Cruithne. Epimetheus and Janus, satellites of Saturn, have a similar relationship, though they are of similar masses and so actually exchange orbits with each other periodically. (Janus is roughly 4 times more massive but still light enough for its orbit to be altered.) Another similar configuration is known as orbital resonance, in which orbiting bodies tend to have periods of a simple integer ratio, due to their interaction. In fictionLagrange points are often mentioned in science fiction (most often hard science fiction), but are rarely used as a plot device because Lagrange points are unfamiliar outside of the scientific or spaceenthusiast community. L1
L2
L3
L4
L5
Unspecified Lagrange points
Related conceptsIn Larry Niven's novel Ringworld, the Puppeteers' "Fleet of Worlds" is arranged in a configuration (5 planets spaced at the points of a pentagon) called a Klemperer Rosette (misspelled "Kemplerer" in the novel). In actual fact, while it is an extension of the Lagrange concept to a special case Nbody problem, and on the surface appears to be an extension of the L4 and L5 orbital mechanics, its stability is more akin to the L1, L2, and L3 positions. Considerable energy expenditure would be required to maintain it over time. See also
Notes and referencesExternal links
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Published  July 2009
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