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An online calculator to compute the precise positions of the 5 Lagrange points for any 2-body system—Tony Dunn; Astronomy Cast—Ep. 76: "Lagrange Points" by Fraser Cain and Pamela L. Gay; The Five Points of Lagrange by Neil deGrasse Tyson; Earth, a lone Trojan discovered
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. [34] [35] WIND: Sun–Earth L 2: NASA: Arrived at L 2 in November 2003 and departed April 2004. Gaia Space Observatory: Sun–Earth L 2: ESA: Launched 19 ...
Lagrange point colonization is a proposed form of space colonization [1] of the five equilibrium points in the orbit of a planet or its primary moon, called Lagrange points. The Lagrange points L 4 and L 5 are stable if the mass of the larger body is at least 25 times the mass of the secondary body. [2] [3] Thus, the points L 4 and L 5 in the ...
[4] [verification needed] A more complex example is the one at right, the Earth's Hill sphere, which extends between the Lagrange points L 1 and L 2, [clarification needed] which lie along the line of centers of the Earth and the more massive Sun. [not verified in body] The gravitational influence of the less massive body is least in that ...
The five equilibrium points of the circular problem are known as the Lagrangian points. See figure below: Restricted three-body problem. In the restricted three-body problem math model figure above (after Moulton), the Lagrangian points L 4 and L 5 are where the Trojan planetoids resided (see Lagrangian point); m 1 is the Sun and m 2 is Jupiter.
The orbits for two of the points, L 4 and L 5, are stable, but the halo orbits for L 1 through L 3 are stable only on the order of months. In addition to orbits around Lagrange points, the rich dynamics that arise from the gravitational pull of more than one mass yield interesting trajectories, also known as low energy transfers. [4]
The name comes from the L 4 and L 5 Lagrangian points in the Earth–Moon system proposed as locations for the huge rotating space habitats that O'Neill envisioned. L 4 and L 5 are points of stable gravitational equilibrium located along the path of the Moon's orbit, 60 degrees ahead or behind it. [2]
The Lagrange points can then be seen as the five places where the gradient on the resultant surface is zero, indicating that the forces are in balance there. [citation needed] In the restricted three-body problem formulation, in the description of Barrow-Green, [4]: 11–14