A Method to Stabilize Ringworlds and Dyson Spheres

Since the concept of Dyson Spheres has been here for many years, it has been the subject of many discussions. When physicist Freeman Dyson first mentioned the idea, he knew that a Dyson Sphere would most probably not consist of a solid sphere but rather be a group of satellites orbiting around a star in a spherical pattern. A key difficulty with the rigid sphere is its instability, which should eventually result in its fall. On the other hand, a recent study presents a different view that suggests a solid Dyson Sphere could be preserved stable if there are certain stable orbits in the vicinity—most notably in a binary star system where there is a great difference in the two star masses.

The concept of a Dyson Sphere was first proposed in 1960 by physicist Freeman Dyson. The Dyson Sphere is a hypothetical structure developed to be the global leader of a star’s energy batch. It could be in the form of a big shell, a flotilla, or a matrix of solar satellites connected with each other. Dyson noted constructing a solid sphere would be infeasible because of the material and stability issues. Instead, a more viable approach involves a Dyson swarm—a collection of orbiting solar power stations capable of harnessing vast amounts of energy.

In the last few years the idea of a solid Dyson sphere has stagnated due to research that has been focused on the detecting of swarms of satellites. The point is that the idea that by using a rigid construction be inherently unstable has been confirmed in many studies. In 1856, James Clerk Maxwell demonstrated that the rings of Saturn could not be a cohesive, solid entity, such as one massive toothed wheel, since the respective gravitational interactions of the planet and rings would cause the latter to collapse. This process was the one that was most believed little would not break, until Colin R. McInnes questioned that idea when he published in the Monthly Notices of the Royal Astronomical Society.

McInnes contends that the real crux of the problem is in the circular restricted three-body problem, a common formulation in orbital and celestial mechanics. This question expresses the motion of a small satellite, e.g. an asteroid that is under the influence of only two larger bodies-e.g. the two bodies in the Sun and Jupiter that move around their common center of mass. The small object, by virtue of its infitesingly small mass, will not, to any great degree, affect the motions of the two larger ones.

In this configuration, there are also five singular points called Lagrange points. What’s more, two of them are not stable initially, while L4, and L5 are still stable as described in the case of the Sun-Jupiter system where the mass ratio between the primary bodies is rather smaller. For instance, the scenario where radiation pressure also affects stability is more complex to be described.

McInnes’ observations indicate that for certain endurances a solid or very dense nucleus could gain stability. The example is supposed to be a huge ring around the smaller of the two central orbits. Additionally, McInnes claims that a closed Dyson sphere could also persist respectively around the smaller of the two bodies in the system.

Source : Ringworlds and Dyson spheres can be stable 

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