Orbital stability in the Solar System for arbitrary inclinations and eccentricities: planetary perturbations versus resonances. (arXiv:1905.05870v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_T/0/1/0/all/0/1">Tabare Gallardo</a>

Applying the technique of dynamical maps we study the orbital stability of
test particles in the Solar System in the space (a,e,i) defined by 0.1

Applying the technique of dynamical maps we study the orbital stability of
test particles in the Solar System in the space (a,e,i) defined by 0.1<a<38 au,
0<e<0.9 and 0<i<180 identifying the unstable and stable regions. We find stable
niches where small bodies can survive even for very high eccentricities. Mean
motion resonances play a fundamental role providing stability against the
planetary perturbations specially for high inclination orbits. A stability
stripe around i=150 is present all along the Solar System. We found that the
population of objects with semimajor axes between 10 and 30 au is evolving
inside a highly unstable region according to our maps. For the inner Solar
System we found that the region between the Hildas and Jupiter is more stable
for high eccentricity orbits than for low eccentricity ones.

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