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From wispy gas giants on the verge of disruption to tiny rocky bodies alreadyfalling apart, short-period exoplanets pose a severe puzzle to theories ofplanet formation and orbital evolution. By far most of the planets known beyondthe solar system orbit their stars in much tighter orbits than the mostclose-in planet in the solar system, Mercury. Short-period planets experienceddynamical and evolutions histories distinct from their farther-out cousins, andso it's not clear they are representative of all planets. These exoplanetstypically have radii between about 1 and 4 Earth radii, whereas the solarsystem does not contain any planet in this radius range. And while the mostmassive planets in the solar system occupy the icy regions beyond about 5 AUfrom the sun, about 1% of sun-like stars have a Jupiter-mass planet near 0.05AU, with just a few days of an orbital period. How did these short-periodplanets get there? Did they form in-situ, or did they migrate towards theircontemporary orbits? If they migrated, what prevented them from falling intotheir stars? Vice versa, could some of the remaining 99% of stars without sucha hot Jupiter show evidence of their past consumption of a close-in, massiveplanet? The proximity between short-period planets and their host starsnaturally facilitates observational studies, and so short-period planetsdominate our observational constraints on planetary composition, internalstructure, meteorology, and more. This white paper discusses the uniqueadvantages of short-period planets for the theoretical and observationalinvestigations of exoplanets in general and of their host stars.

Investigating Planet Formation and Evolutionary Processes with Short-Period Exoplanets