High-resolution resonant portraits of a single-planet white dwarf system

ABSTRACT The dynamical excitation of asteroids due to mean motion resonant interactions with planets is enhanced when their parent star leaves the main sequence. However, numerical investigation outcomes within post-main-sequence simulations computationally expensive, limiting extent which detailed analyses have been performed. Here, we combine use a high-performance computer cluster and general semi-analytical libration width formulation Gallardo, Beaugé & Giuppone in order quantify stability, strength, variation instigated by stellar evolution for single-planet system containing on both crossing non-crossing orbits. We find that instability can be accurately bound only main-sequence values computing maximum as function asteroid longitude pericentre. also relative efficiency resonances different orders stabilize versus destabilize orbits during giant branch white dwarf phases. 4:1, 3:1, 2:1 represent efficient polluters dwarfs, even orbit-crossing regime, 4:3 3:2 retain small reservoirs stable throughout evolution. This represents preliminary step characterizing how simplified extrasolar Kirkwood gap structures evolve beyond