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Post-main-sequence planetary system evolution
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Post-main-sequence planetary system evolution
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The fates of planetary systems provide unassailable insights into their formation and represent rich cross-disciplinary dynamical laboratories. Mounting observations of post-main-sequence planetary systems necessitate a complementary level of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the interpretation and modelling of currently known systems and upcoming discoveries.
Forward citations
Cited by 2 Pith papers
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Magnetically guided accretion and extremely slow rotation in a metal-enriched white dwarf
WD 1532+129 rotates once every ~289 days — the slowest directly measured spin of any white dwarf — and its accreted metals sit in patches at both magnetic poles.
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Dynamical constraints on planet engulfment as the origin of lithium enhancement in TOI-5882
In 300 MESA+REBOUND runs of TOI-5882, planet engulfment is the most common outcome, yet only ~5% fall inside the Li-detectable subgiant window, so recent engulfment remains viable but non-generic under the explored setups.
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