Instabilities in compact planetary systems are generically driven by chaotic dynamics. This implies that an instability time measured through direct N-body integration is not exact, but rather represents a single draw from a distribution of equally valid chaotic trajectories.
As discoveries of terrestrial, Earth-sized exoplanets that lie within the habitable zone of their host stars continue to occur at increasing rates, efforts have began to shift from the detection of these worlds to the characterization of their atmospheres through transit spectroscopy.
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