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The large number of exoplanets found to orbit their host stars in very closeorbits have significantly advanced our understanding of the planetary formationprocess. It is now widely accepted that such short-period planets cannot haveformed {\em in situ}, but rather must have migrated to their current orbitsfrom a formation location much farther from their host star. In the late stagesof planetary formation, once the gas in the proto-planetary disk has dissipatedand migration has halted, gas-giants orbiting in the inner disk regions willexcite planetesimals and planetary embryos, resulting in an increased rate oforbital crossings and large impacts. We present the results of dynamicalsimulations for planetesimal evolution in this later stage of planet formation.We find that a mechanism is revealed by which the collision-merger of planetaryembryos can kick terrestrial planets directly into orbits extremely close totheir parent stars.

Forming Close-in Earth-like Planets via a Collision-Merger Mechanism in Late-stage Planet Formation