2001/01/09 by E. Gueron, P. S. Letelier
Physics and Astronomy · #astro-ph #gr-qc #nlin.CD
paper · pdf · doi:10.1051/0004-6361:20010018
published as Astron.Astrophys. 368 (2001) 716-720 · RevTEX, 7 eps figures, to appear in Astron Astrophys
arxiv created 2001/01/09 · arxiv updated 2009/11/30
The Newtonian as well as the special relativistic dynamics are used to study the stability of orbits of a test particle moving around a black hole plus a dipolar halo. The black hole is modeled by either the usual monopole potential or the Paczynki-Wiita pseudo-Newtonian potential. The full general relativistic similar case is also considered. The Poincare section method and the Lyapunov characteristic exponents show that the orbits for the pseudo-Newtonian potential models are more unstable than the corresponding general relativistic geodesics.