DPS 2001 meeting, November 2001
Session 29. Rings I
Oral, Chair: L. Spiker, Thursday, November 29, 2001, 11:40am-12:40pm, Regency GH

[Previous] | [Session 29] | [Next]

[29.04] Coorbital particles under the effects of Poynting-Robertson Drag

S. M. Giuliatti Winter, O. C. Winter, A.H.F. Guimar„es (UNESP-Brazil)

The confinement model as proposed by Dermott et al. (Icarus, 1980) explained the stability of narrow planetary rings through the presence of a small satellite (\mu < 10-10) embedded in the ring, where the particles are maintained in horseshoe orbits. They proposed that such configuration is stable even in the presence of Poynting-Robertson (PR) drag. Murray (Icarus, 1994) analysed the location and stability of the Lagrangian points under the effects of different types of drag forces and concluded that for heliocentric orbits the triangular equilibrium points are unstable under PR drag. The analysis was made for small amplitude orbits. In the present work we explore the dynamics of particles coorbital with a satellite of Saturn under the effects of the PR drag. Therefore, we are considering a planetocentric problem. Different values of satellite mass (10-6-10-11mSaturn) and particle size (0.1--10\mum) are taken into account. The range of the initial conditions covers small and large amplitude orbits. Our results show that when the PR Drag is intense (small particle and/or small satellite) the trajectory of the particle is chaotic or it collides with the satellite. The trajectory changes intermittently between tadpole and horseshoe orbits of different radial and angular amplitudes. There is a difference between the dynamical stability of the equilateral Lagrangian points, which depends on the PR Drag intensity. In general, the Lagrangian point L5 is more stable than L4.

Acknowledgements: SMGW, OCW and AHFG thanks FAPESP and OCW also thanks CNPq for the financial support.

[Previous] | [Session 29] | [Next]