### Rosette orbit

A **Klemperer rosette** is a gravitational system of heavier and lighter bodies orbiting in a regular repeating pattern around a common barycenter. It was first described by W. B. Klemperer in 1962.^{[1]}

Klemperer described the system as follows: Template:Cquote The simplest rosette would be series of four alternating heavier and lighter bodies, 90 degrees from one another, in a rhombic configuration [Heavy, Light, Heavy, Light], where the two heavier masses weigh the same, and likewise the two lighter masses weigh the same. The number of "mass types" can be increased, so long as the arrangement pattern is cylic: e.g. [ 1,2,3 ... 1,2,3 ], [ 1,2,3,4,5 ... 1,2,3,4,5 ], [ 1,2,3,3,2,1 ... 1,2,3,3,2,1 ] etc. Klemperer also mentioned octagonal and rhombic rosettes. While all Klemperer rosettes are vulnerable to destablization (read below), the hexagonal rosette (as in the diagram to the right) should have extra stability due to the 'planets' sitting in each others' L4 and L5 Lagrangian points.

## Misuse and misspelling

The term "Klemperer rosette" (often misspelled "*Kemplerer* rosette") is often used to mean a configuration of three or more equal masses, set at the points of an equilateral polygon and given an equal angular velocity about their center of mass.
Klemperer does indeed mention this configuration at the start of his article, but only as an already known set of equilibrium systems before introducing the actual rosettes.

In Larry Niven's novel *Ringworld*, the Puppeteers' "Fleet of Worlds" is arranged in such a configuration (5 planets spaced at the points of a pentagon) which Niven calls a "Kemplerer rosette"; this (possibly intentional) misspelling (and misuse) is one possible source of this confusion. Another is the similarity between Klemperer's name and that of Johannes Kepler, who described certain laws of planetary motion in the 17th century. It is notable that these fictional planets were maintained in position by large engines in addition to gravitational force.

## Instability

Simulations of this system^{[2]} (or a simple linear perturbation analysis) demonstrate that such systems are definitely **not** stable: any motion away from the perfect geometric configuration causes an oscillation, eventually leading to the disruption of the system (Klemperer's original article also states this fact). This is the case whether the center of the Rosette is in free space, or itself in orbit around a star. The short-form reason is that any perturbation destroys the symmetry, which increases the perturbation, which further damages the symmetry, and so on.

The longer explanation is that any tangential perturbation causes a body to get closer to one neighbor and farther from another; the gravitational force becomes greater towards the closer neighbor and less for the farther neighbor, pulling the perturbed object further towards its closer neighbor, enhancing the perturbation rather than damping it. An inward radial perturbation causes the perturbed body to get closer to *all* other objects, increasing the force on the object and increasing its orbital velocityâ€”which leads indirectly to a tangential perturbation and the argument above.

## References

## External links

- Rosette simulations using Java applets
- Kemplerer (Klemperer) Rosette by Larry Niven from Ringworld