A Klemperer rosette is a gravitational system of (optionally) alternating heavier and lighter bodies orbiting in a symmetrical pattern around a common barycenter. It was first described by W.B. Klemperer in 1962, and is a special case of a central configuration.
Klemperer described rosette systems as follows:
In astrodynamics, the orbital eccentricity of an astronomical object is a dimensionless parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabolic (escape orbit or capture orbit), and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a rosette orbit through the Galaxy.
Dr. Wolfgang Benjamin Klemperer (January 18, 1893 – March 25, 1965) was born in Dresden, Germany, the son of the Austrian nationals Leon and Charlotte Klemperer. He was in his time a prominent aviation and aerospace scientist and engineer, who ranks among the pioneers of early aviation.
He is probably best known for his work on Properties of Rosette Configurations of Gravitating Bodies in Homographic Equilibrium, which have been named after him as Klemperer rosettes.