Abstract We have presented in this communication a new solving procedure for the dynamics of non-rigid asteroid rotation, considering the final spin state of rotation for a small celestial body (asteroid). The last condition means the ultimate absence of the applied external torques (including short-term effect from torques during collisions, long-term YORP effect, etc.). Fundamental law of angular momentum conservation has been used for the aforementioned solving procedure. The system of Euler equations for dynamics of non-rigid asteroid rotation has been explored with regard to the existence of an analytic way of presentation of the approximated solution. Despite of various perturbations (such as collisions, YORP effect) which destabilize the rotation of asteroid via deviating from the current spin state, the inelastic (mainly, tidal) dissipation reduces kinetic energy of asteroid. So, evolution of the spinning asteroid should be resulting by the rotation about maximal-inertia axis with the proper spin state corresponding to minimal energy with a fixed angular momentum. Basing on the aforesaid assumption (component K 1 is supposed to be fluctuating near the given appropriate constant of the fixed angular momentum), we have obtained that 2-nd component K 2 is the solution of appropriate Riccati ordinary differential equation of 1-st order, whereas component K 3 should be determined via expression for K 2.
Highlights The dynamics of asteroid rotation moving along the elliptic orbit is explored. New type of solutions for dynamics of non-rigid asteroid rotation are obtained. New method for solving Euler's equations of non-rigid body rotation is suggested. Evolution of spin towards rotation about maximal-inertia axis is approximated. The 2-nd component of angular momentum is proved to be solution of Riccati ODE.
On the dynamics OF NON-RIGID asteroid rotation
Acta Astronautica ; 161 ; 40-43
2019-05-04
4 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
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