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Sub-Neptunes around FGKM dwarfs are evenly distributed in log orbital perioddown to $\sim$10 days, but dwindle in number at shorter periods. Both the breakat $\sim$10 days and the slope of the occurrence rate down to $\sim$1 day canbe attributed to the truncation of protoplanetary disks by their host starmagnetospheres at co-rotation. We demonstrate this by deriving planetoccurrence rate profiles from empirical distributions of pre-main-sequencestellar rotation periods. Observed profiles are better reproduced when planetsare distributed randomly in disks---as might be expected if planets formed insitu---rather than piled up near disk edges, as would be the case if theymigrated in by disk torques. Planets can be brought from disk edges toultra-short ($< 1$ day) periods by asynchronous equilibrium tides raised ontheir stars. Tidal migration can account for how ultra-short period planets(USPs) are more widely spaced than their longer period counterparts. Ourpicture provides a starting point for understanding why metal-rich stars tendto harbor more USPs, and why the sub-Neptune population drops at $\sim$10 daysregardless of whether the host star is of type FGK or early M. We predictplanet occurrence rates around A stars to also break at short periods, but at$\sim$1 day instead of $\sim$10 days because A stars rotate faster than lowermass stars (this prediction presumes that the planetesimal building blocks ofplanets can drift inside the dust sublimation radius).

Magnetospheric Truncation, Tidal Inspiral, and the Creation of Short and Ultra-Short Period Planets