Systems of Colliding Bodies in a Gravitational Field  Evolution and Role of the Internal Rotations
Abstract
To emphasize the rotational effects of a simple friction between colliding bodies in a keplerian field we investigate numerically the evolution of the rotational energies in a three dimensional system of spherical particles interacting through inelastic collisions in a deterministic model. All the particles are made of the same material but they possibly have different sizes. Each collision reduces the relative surface velocity and there are exchanges between orbital energy and rotational energy. Our results are compared with some previous papers and our aim is to supply other probabilists models with simple basic references about mean dynamical properties. The rotational energy of the colliding bodies tends to reach an equilibrium state that depends only on the rate of energy loss in the collision process. Internal rotations prevent the complete flattening of the system. With this model, light and small particles spin faster than the massive and big ones. We observe an excess of prograde rotations on counterclockwise orbits. The ratio of rotational and orbital energies is 2!1!+% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9LqJc9% vqaqpepm0xbba9pwe9Q8fs0yqaqpepae9pg0FirpepeKkFr0xfrx% frxb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaGaamyramaaBa% aaleaacaWGYbaabeaakiaac+cacaWGfbWaaSbaaSqaaiaadUgaaeqa% aOGaeyisISRaaGymaiaaicdadaahaaWcbeqaaiabgkHiTiaaiodaaa% aaaa!3F83![E_r /E_k ≈ 10^{  3} ] while the ratio of corresponding mean angular velocities is 2!1!+% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXatLxBI9gBaerbd9wDYLwzYbItLDharqqtubsr% 4rNCHbGeaGqiVu0Je9sqqrpepC0xbbL8F4rqqrFfpeea0xe9LqJc9% vqaqpepm0xbba9pwe9Q8fs0yqaqpepae9pg0FirpepeKkFr0xfrx% frxb9adbaqaaeGaciGaaiaabeqaamaabaabaaGcbaWaaaWaaeaacq% aHjpWDaiaawMYicaGLQmcacaGGVaWaaaWaaeaacqGHPoWvaiaawMYi% caGLQmcacqGHijYUcaaIYaaaaa!4008![left< ω rightrangle /left< Ω rightrangle ≈ 2] These values depends strongly on the dimensional scale of the model.
 Publication:

Earth Moon and Planets
 Pub Date:
 September 1992
 DOI:
 10.1007/BF00057853
 Bibcode:
 1992EM&P...58..271C
 Keywords:

 Gravitational Fields;
 Inelastic Collisions;
 Kepler Laws;
 Rotating Bodies;
 Angular Momentum;
 Cosmology;
 Many Body Problem;
 Orbital Mechanics;
 Three Dimensional Models;
 Astrophysics