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The ability of a planet to maintain surface water, key to life as we know it,depends on solar and planetary energy. As a star ages, it delivers more energyto a planet. As a planet ages it produces less internal heat, which leads tocooling. For the Earth, interior cooling connects to plate tectonics - thesurface manifestation of convection within the Earth's interior. This processcycles volatiles (CO2 and water) between surface and interior reservoirs, whichaffects planetary climate. Cycling rates depend on the efficiency of platetectonic cooling. That efficiency remains debated and multiple hypotheses havebeen put forth. Geological proxy data allow us to validate these hypothesesaccounting for model and data uncertainty. Multiple models pass the validationtest. Those models define a distribution for terrestrial exoplanets akin toEarth, accounting for variations in tectonic efficiency. Feeding thisdistribution into climate models indicates that the time at which habitableconditions are established can vary by billions of years. Planets of the sameabsolute age and orbital distance can reside and not reside within the classichabitable zone due to differences in plate tectonic cooling efficiencies. Thefull model population allows a probability distribution to be constructed forthe the time at which habitable conditions are established. The distributionindicates that Earth-like exoplanets, of the same age, can be at differentevolutionary stages. It also indicates that planets around stars whose earlyevolution is unfavorable for life can become habitable later in their energetichistories.

The Temporal Onset of Habitability For Earth-Like Planets