In celestial mechanics, the Lagrangian points (/ləˈɡrɑːndʒiən/; also Lagrange points, L-points, or libration points) are positions in an orbital configuration of two large bodies where a small object affected only by gravity can maintain a stable position relative to the two large bodies. The Lagrange points mark positions where the combined gravitational pull of the two large masses provides precisely the centripetal force required to orbit with them. There are five such points, labeled L1 to L5, all in the orbital plane of the two large bodies. The first three are on the line connecting the two large bodies; the last two, L4 and L5, each form an equilateral triangle with the two large bodies. The two latter points are stable, which implies that objects can orbit around them in a rotating coordinate system tied to the two large bodies.
Several planets have satellites near their L4 and L5 points (trojans) with respect to the Sun, with Jupiter in particular having more than a million of these. Artificial satellites have been placed at L1 and L2 with respect to the Sun and Earth, and Earth and the Moon, for various purposes, and the Lagrangian points have been proposed for a variety of future uses in space exploration.
The three collinear Lagrange points (L1, L2, L3) were discovered by Leonhard Euler a few years before Lagrange discovered the remaining two.
In 1772, Joseph-Louis Lagrange published an "Essay on the three-body problem". In the first chapter he considered the general three-body problem. From that, in the second chapter, he demonstrated two special constant-pattern solutions, the collinear and the equilateral, for any three masses, with circular orbits.
The five Lagrangian points are labeled and defined as follows:
The L1 point lies on the line defined by the two large masses M1 and M2, and between them. It is the most intuitively understood of the Lagrangian points: the one where the gravitational attraction of M2 partially cancels M1's gravitational attraction.
The L2 point lies on the line through the two large masses, beyond the smaller of the two. Here, the gravitational forces of the two large masses balance the centrifugal effect on a body at L2.
The L3 point lies on the line defined by the two large masses, beyond the larger of the two.
The L4 and L5 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 (L5) or ahead (L4) of the smaller mass with regard to its orbit around the larger mass.
The triangular points (L4 and L5) are stable equilibria, provided that the ratio of M1/ is greater than 24.96. This is the case for the Sun–Earth system, the Sun–Jupiter system, and, by a smaller margin, the Earth–Moon system. When a body at these points is perturbed, it moves away from the point, but the factor opposite of that which is increased or decreased by the perturbation (either gravity or angular momentum-induced speed) will also increase or decrease, bending the object's path into a stable, kidney-bean-shaped orbit around the point (as seen in the corotating frame of reference).
In contrast to L4 and L5, where stable equilibrium exists, the points L1, L2, and L3 are positions of unstable equilibrium. Any object orbiting at L1, L2, or L3 will tend to fall out of orbit; it is therefore rare to find natural objects there, and spacecraft inhabiting these areas must employ station keeping in order to maintain their position.
It is common to find objects at or orbiting the L4 and L5 points of natural orbital systems. These are commonly called "trojans"; in the 20th century, asteroids discovered orbiting at the Sun–Jupiter L4 and L5 points were named after characters from Homer's Iliad. Asteroids at the L4 point, which leads Jupiter, are referred to as the "Greek camp", whereas those at the L5 point are referred to as the "Trojan camp". See also Trojan (astronomy).
Other examples of natural objects orbiting at Lagrange points:
Lagrangian points are the constant-pattern solutions of the restricted three-body problem. For example, given two massive bodies in orbits around their common barycenter, there are five positions in space where a third body, of comparatively negligible mass, could be placed so as to maintain its position relative to the two massive bodies. As seen in a rotating reference frame that matches the angular velocity of the two co-orbiting bodies, the gravitational fields of two massive bodies combined with the minor body's centrifugal force are in balance at the Lagrangian points, allowing the smaller third body to be relatively stationary with respect to the first two.
The location of L1 is the solution to the following equation, balancing gravitation and the centrifugal force:
where r is the distance of the L1 point from the smaller object, R is the distance between the two main objects, and M1 and M2 are the masses of the large and small object, respectively. (The quantity in parentheses on the right is the distance of L1 from the center of mass.) Solving this for r involves solving a quintic function, but if the mass of the smaller object (M2) is much smaller than the mass of the larger object (M1) then L1 and L2 are at approximately equal distances r from the smaller object, equal to the radius of the Hill sphere, given by:
This distance can be described as being such that the orbital period, corresponding to a circular orbit with this distance as radius around M2 in the absence of M1, is that of M2 around M1, divided by √ ≈ 1.73:
The location of L2 is the solution to the following equation, balancing gravitation and inertia:
with parameters defined as for the L1 case. Again, if the mass of the smaller object (M2) is much smaller than the mass of the larger object (M1) then L2 is at approximately the radius of the Hill sphere, given by:
The location of L3 is the solution to the following equation, balancing gravitation and the centrifugal force:
with parameters defined as for the L1 and L2 cases except that r now indicates how much closer L3 is to the more massive object than the smaller object. If the mass of the smaller object (M2) is much smaller than the mass of the larger object (M1) then:
The reason these points are in balance is that, at L4 and L5, 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 three-body system, this resultant force is exactly that required to keep the smaller body at the Lagrange point in orbital equilibrium with the other two larger bodies of system. (Indeed, the third body need not have negligible mass.) The general triangular configuration was discovered by Lagrange in work on the three-body problem.
The radial acceleration a of an object in orbit at a point along the line passing through both bodies is given by:
Where r is the distance from the large body M1. The terms in this function represent respectively: force from M1; force from M2; and centrifugal force. The points L3, L1, L2 occur where the acceleration is zero — see chart at right.
Although the L1, L2, and L3 points are nominally unstable, there are (unstable) periodic orbits called "halo" orbits around these points in a three-body system. A full n-body dynamical system such as the Solar System does not contain these periodic orbits, but does contain quasi-periodic (i.e. bounded but not precisely repeating) orbits following Lissajous-curve trajectories. These quasi-periodic Lissajous orbits are what most of Lagrangian-point space missions have used until now. Although they are not perfectly stable, a modest effort of station keeping keeps a spacecraft in a desired Lissajous orbit for a long time. Also, for Sun–Earth-L1 missions, it is preferable for the spacecraft to be in a large-amplitude (100,000–200,000 km or 62,000–124,000 mi) Lissajous orbit around L1 than to stay at L1, because the line between Sun and Earth has increased solar interference on Earth–spacecraft communications. Similarly, a large-amplitude Lissajous orbit around L2 keeps a probe out of Earth's shadow and therefore ensure a better illumination of its solar panels.
This table lists sample values of L1, L2, and L3 within the solar system. Calculations assume the two bodies orbit in a perfect circle with separation equal to the semimajor axis and no other bodies are nearby. Distances are measured from the larger body's center of mass with L3 showing a negative location. The percentage columns show how the distances compare to the semimajor axis. E.g. for the Moon, L1 is located 400 km from Earth's center, which is 84.9% of the Earth-Moon distance or 15.1% in front of the Moon; L2 is located 326900 km from Earth's center, which is 116.8% of the Earth-Moon distance or 16.8% beyond the Moon; and L3 is located 448700 km from Earth's center, which is 99.3% of the Earth-Moon distance or 0.7084% in front of the Moon's 'negative' position. The L3 percent value has been magnified by 100. −381
|Body pair||Semimajor axis (SMA)||L1||1-L1/SMA %||L2||L2/SMA-1 %||L3||(1+L3/SMA)*100 %|
|Earth-Moon||×108 m3.844||×108 m3.2639||15.09||×108 m4.489||16.78||×108 m−3.8168||0.7084|
|Sun-Mercury||×1010 m5.7909||×1010 m5.7689||0.3806||×1010 m5.813||0.3815||×1010 m−5.7909||96830.000|
|Sun-Venus||×1011 m1.0821||×1011 m1.072||0.9315||×1011 m1.0922||0.9373||×1011 m−1.0821||280.014|
|Sun-Earth||×1011 m1.496||×1011 m1.4811||0.997||×1011 m1.511||1.004||×1011 m−1.496||520.017|
|Sun-Mars||×1011 m2.2794||×1011 m2.2686||0.4748||×1011 m2.2903||0.4763||×1011 m−2.2794||8820.001|
|Sun-Jupiter||×1011 m7.7834||×1011 m7.2645||6.667||×1011 m8.3265||6.978||×1011 m−7.7791||5.563|
|Sun-Saturn||×1012 m1.4267||×1012 m1.3625||4.496||×1012 m1.4928||4.635||×1012 m−1.4264||1.667|
|Sun-Uranus||×1012 m2.8707||×1012 m2.8011||2.421||×1012 m2.9413||2.461||×1012 m−2.8706||0.2546|
|Sun-Neptune||×1012 m4.4984||×1012 m4.3834||2.557||×1012 m4.6154||2.602||×1012 m−4.4983||0.3004|
Sun–Earth L1 is suited for making observations of the Sun–Earth system. Objects here are never shadowed by Earth or the Moon and, if observing Earth, always view the sunlit hemisphere. The first mission of this type was the International Sun Earth Explorer 3 (ISEE-3) mission used as an interplanetary early warning storm monitor for solar disturbances. Since June 2015, DSCOVR has orbited the L1 point.
Sun–Earth L2 is a good spot for space-based observatories. Because an object around L2 will maintain the same relative position 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 at L2. (Real spacecraft generally orbit around L2, avoiding partial eclipses of the Sun to maintain a constant temperature). From locations near L2, the Sun, Earth and Moon are relatively close together in the sky; this means that a large sunshade with the telescope on the dark-side can allow the telescope to cool passively to around 50 K – this is especially helpful for infrared astronomy and observations of the cosmic microwave background.
Sun–Earth L3 was a popular place to put a "Counter-Earth" in pulp science fiction and comic books. Once space-based observation became possible via satellites and probes, it was shown to hold no such object. The Sun–Earth L3 is unstable and could not contain a natural object, large or small, for very long. This is because the gravitational forces of the other planets are stronger than that of Earth (Venus, for example, comes within 0.3 AU of this L3 every 20 months).
A spacecraft orbiting near Sun–Earth L3 would be able to closely monitor the evolution of active sunspot regions before they rotate into a geoeffective position, so that a 7-day early warning could be issued by the NOAA Space Weather Prediction Center. Moreover, a satellite near Sun–Earth L3 would provide very important observations not only for Earth forecasts, but also for deep space support (Mars predictions and for manned mission to near-Earth asteroids). In 2010, spacecraft transfer trajectories to Sun–Earth L3 were studied and several designs were considered.
Missions to Lagrangian points generally orbit the points rather than occupy them directly.
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.
Earth–Moon L1 allows comparatively easy access to Lunar and Earth orbits with minimal change in velocity and this has as an advantage to position a half-way manned space station intended to help transport cargo and personnel to the Moon and back.
Earth–Moon L2 would be a good location for a communications satellite covering the Moon's far side and would be "an ideal location" for a propellant depot as part of the proposed depot-based space transportation architecture.
Scientists at the B612 Foundation are planning to use Venus's L3 point to position their planned Sentinel telescope, which aims to look back towards Earth's orbit and compile a catalogue of near-Earth asteroids.
International Sun Earth Explorer 3 (ISEE-3) began its mission at the Sun–Earth L1 before leaving to intercept a comet in 1982. The Sun–Earth L1 is also the point to which the Reboot ISEE-3 mission was attempting to return the craft as the first phase of a recovery mission (as of September 25, 2014 all efforts have failed and contact was lost).
Deep Space Climate Observatory (DSCOVR), launched on 11 February 2015, began orbiting L1 on 8 June 2015 to study the solar wind and its effects on Earth. DSCOVR is unofficially known as GORESAT, because it carries a camera always oriented to Earth and capturing full-frame photos of the planet similar to the Blue Marble. This concept was proposed by then-Vice President of the United States Al Gore in 1998 and was a centerpiece in his film An Inconvenient Truth.
LISA Pathfinder (LPF) was launched on 3 December 2015, and arrived at L1 on 22 January 2016, where, among other experiments, it will test the technology needed by (e)LISA to detect gravitational waves. LISA Pathfinder uses an instrument consisting of two small gold alloy cubes.
|– Unflown or planned mission||– Mission en route or in progress (including mission extensions)||– Mission at Lagrangian point completed successfully (or partially successfully)|
|International Sun–Earth Explorer 3 (ISEE-3)||Sun–Earth L1||NASA||Launched in 1978, it was the first spacecraft to be put into orbit around a libration point, where it operated for four years in a halo orbit about the L1 Sun–Earth point. After the original mission ended, it was commanded to leave L1 in September 1982 in order to investigate comets and the Sun. Now in a heliocentric orbit, an unsuccessful attempt to return to halo orbit was made in 2014 when it made a flyby of the Earth–Moon system.|
|Advanced Composition Explorer (ACE)||Sun–Earth L1||NASA||Launched 1997. Has fuel to orbit near L1 until 2024. Operational as of 2016[update].|
|Deep Space Climate Observatory (DSCOVR)||Sun–Earth L1||NASA||Launched on 11 February 2015. Planned successor of the Advanced Composition Explorer (ACE) satellite. Operational as of 2016[update].|
|LISA Pathfinder (LPF)||Sun–Earth L1||ESA, NASA||Launched one day behind revised schedule (planned for the 100th anniversary of the publication of Einstein's General Theory of Relativity), on 3 December 2015. Arrived at L1 on 22 January 2016.|
|Solar and Heliospheric Observatory (SOHO)||Sun–Earth L1||ESA, NASA||Orbiting near L1 since 1996. Operational as of 2013[update].|
|WIND||Sun–Earth L1||NASA||Arrived at L1 in 2004 with fuel for 60 years. Operational as of 2017[update].|
|Wilkinson Microwave Anisotropy Probe (WMAP)||Sun–Earth L2||NASA||Arrived at L2 in 2001. Mission ended 2010, then sent to solar orbit outside L2.|
|Herschel Space Telescope||Sun–Earth L2||ESA||Arrived at L2 July 2009. Ceased operation on 29 April 2013; will be moved to a heliocentric orbit.|
|Planck Space Observatory||Sun–Earth L2||ESA||Arrived at L2 July 2009. Mission ended on 23 October 2013; Planck has been moved to a heliocentric parking orbit.|
|Chang'e 2||Sun–Earth L2||CNSA||Arrived in August 2011 after completing a lunar mission before departing en route to asteroid 4179 Toutatis in April 2012.|
|Chang'e 5-T1 service module||Earth–Moon L2||CNSA||Arrived in a Lissajous orbit with period of 14 days around the EM-L2 point on November 27, 2014 after its primary mission, the re-entry demonstration of the sample return capsule was completed. It left the EM-L2 orbit on January 4, 2015 and returned to lunar orbit on January 13.|
|ARTEMIS mission extension of THEMIS||Earth–Moon L1 and L2||NASA||Mission consists of two spacecraft, which were the first spacecraft to reach Earth–Moon Lagrangian points. Both moved through Earth–Moon Lagrangian points, and are now in lunar orbit.|
|WIND||Sun–Earth L2||NASA||Arrived at L2 in November 2003 and departed April 2004.|
|Gaia Space Observatory||Sun–Earth L2||ESA||Launched 19 December 2013. Operational as of 24 January 2017.|
|"Lunar Far-Side Communication Satellites"||Earth–Moon L2||NASA||Proposed in 1968 for communications on the far side of the Moon during the Apollo program,
mainly to enable an Apollo landing on the far side—neither the satellites nor the landing were ever realized.
|Space colonization and manufacturing||Earth–Moon L4 or L5||—||First proposed in 1974 by Gerard K. O'Neill and subsequently advocated by the L5 Society.|
|Aditya||Sun–Earth L1||ISRO||Launch planned for 2019–20; it will be going to a point 1.5 million kilometers away from Earth, from where it will
observe the Sun constantly and study the solar corona, the region around the Sun's surface.
|James Webb Space Telescope (JWST)||Sun–Earth L2||NASA, ESA, CSA||As of 2013[update], launch is planned for October 2018.|
|EQUULEUS||Earth-Moon L2||University of Tokyo, JAXA||6U CubeSat, launch planned for December 2018 as a secondary payload onboard SLS Exploration Mission 1.|
|Euclid||Sun–Earth L2||ESA, NASA||As of 2013[update], launch is planned in 2020.|
|Demonstration and Experiment of Space Technology
for INterplanetary voYage (DESTINY)
|Earth–Moon L2||JAXA||Candidate for JAXA's next "Competitively-Chosen Medium-Sized Focused Mission",
possible launch in the early 2020s.
|Exploration Gateway Platform||Earth–Moon L2||NASA||Proposed in 2011.|
|Wide Field Infrared Survey Telescope (WFIRST)||Sun–Earth L2||NASA, USDOE||As of 2013[update], in a "pre-formulation" phase until at least early 2016; possible launch in the early 2020s.|
|LiteBIRD||Sun–Earth L2||JAXA, NASA||As of 2015[update], one of two finalists for JAXA's next "Strategic Large Mission"; would be launched in 2024 if selected.|
|Planetary Transits and Oscillations of stars (PLATO)||Sun–Earth L2||ESA||Planned for launch in 2024 for an initial six-year mission.|
|Space Infrared Telescope for Cosmology
and Astrophysics (SPICA)
|Sun–Earth L2||JAXA, ESA, SRON||As of 2015[update], awaiting approval from both Japanese and European side, launch proposed for 2025.|
|Advanced Telescope for High Energy Astrophysics
|Sun–Earth L2||ESA||Launch planned for 2028.|
Content from Wikipedia