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The Lagrange Points

Orbital sweet spots

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The Lagrange Points

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Lagrange Points are five special points where an object can orbit at a fixed distance from two larger mass such that the gravitational pull precisely equals the centripetal force.
Introduction to Astronomy Series
  1. Introduction to Astronomy
  2. The Celestial Sphere - Right Ascension and Declination
  3. What is Angular Size?
  4. What is the Milky Way?
  5. The Magnitude Scale
  6. Sidereal Time, Civil Time and Solar Time
  7. Equinoxes and Solstices
  8. Parallax, Distance and Parsecs
  9. Flux
  10. Luminosity of Stars
  11. Apparent Magnitude, Absolute Magnitude and Distance
  12. Variable Stars
  13. Spectroscopy and Spectrometry
  14. Redshift and Blueshift
  15. Spectral Classification of Stars
  16. Hertzsprung-Russell Diagram
  17. Kepler's Laws of Planetary Motion
  18. The Lagrange Points
  19. What is an Exoplanet?
  20. Glossary of Astronomy & Photographic Terms

The Lagrange Points were discovered by the Italian-French mathematician Joseph-Louis Lagrange.

There are five Lagrange points to be found in the vicinity of two orbiting masses. Of the five Lagrange points, three are unstable and two are stable. The unstable Lagrange points - labelled L1, L2 and L3 - lie along the line connecting the two large masses. The stable Lagrange points - labelled L4 and L5 - form the apex of two equilateral triangles that have the large masses at their vertices.

Sun-Earth Lagrange points. The STEREO probes are about to pass through L4 and L5. Solar observatories often park themselves at L1 while deep space observatories prefer L2.

Lagrange points 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.

Lagrangian points are the stationary solutions of the circular restricted three-body problem. For example, given two massive bodies in circular orbits around their common centre 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 co-orbiting bodies, the gravitational fields of two massive bodies combined with the satellite's circular motion are in balance at the Lagrangian points, allowing the third body to be stationary with respect to the first two bodies.

The first three Lagrange points are nominally unstable. While it is possible to find stable periodic orbits around these points, if an object located at the L1 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.

In contrast to the unstable Lagrangian points, the triangular points (L4 and L5) are stable, provided that the ratio of M1/M2 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 shown in the contour lines in the image below.

A contour plot of the effective potential of a two-body system. (the Sun and Earth here), showing the 5 Lagrange points. An object in free-fall would trace out a contour (such as the Moon, shown)
Image Credit: Wikipedia
A contour plot of the effective potential of a two-body system. (the Sun and Earth here), showing the 5 Lagrange points. An object in free-fall would trace out a contour (such as the Moon, shown)

L4 and L5 are sometimes called triangular Lagrange points or Trojan points. The name Trojan points comes from the Trojan asteroids at the Sun-Jupiter L4 and L5 points, which themselves are named after characters from Homer's Iliad (the legendary siege of Troy). Asteroids at the L4 point, which leads Jupiter, are referred to as the "Greek camp", while at the L5 point they are referred to as the "Trojan camp". These asteroids are (largely) named after characters from the respective sides of the Trojan War.

Trojan asteroids of Jupiter (coloured green) in front of (the
Image Credit: Wikipedia
Trojan asteroids of Jupiter (coloured green) in front of (the "Greeks") and behind Jupiter along its orbital path. Also shown is the main asteroid belt between the orbits of Mars and Jupiter (white), and the Hilda family of asteroids (brown).


Lagrangian Point Missions

The 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.

MissionLagrangian pointAgencyStatus
Advanced Composition Explorer (ACE)Sun-Earth L1NASAOperational
Solar and Heliospheric Observatory (SOHO)Sun-Earth L1ESA, NASAOperational
WINDSun-Earth L1NASAOperational
International Sun/Earth Explorer 3 (ISEE-3)Sun-Earth L1NASAOriginal mission ended, left L1 point
Wilkinson Microwave Anisotropy Probe (WMAP)Sun-Earth L2NASAOperational
Herschel and Planck Space ObservatoriesSun-Earth L2ESAOperational
ARTEMIS mission extension of THEMISEarth-Moon L1 and L2NASAOperational

Last updated on: Friday 8th September 2017

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