Abstract

The transit yields of the Kepler mission have provided constraints on the demographics of exoplanets around FGK dwarfs, including the number of such systems with multiple transiting planets. Transit multiplicities, in turn, provide insights into the orbital architectures of these systems. Folding in stellar age information from isochrones fit to stars from Gaia enables a study of the timescales along which these observed architectures may have been shaped. By forward modeling planetary systems around FGK dwarfs against the Kepler transit multiplicity around such stars, we begin to rule out and favor certain timescales for the dynamical evolution of exoplanet orbits around Sun-like stars – and the dynamical processes that occur along those timescales. Our findings provide an upper runtime bound on expensive N-body simulations for orbital evolution, as well as a lower bound for the time at which life might emerge in systems around stars similar to the Sun.