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From optical spectroscopic measurements we determine that the HD 15407 binarysystem is ~80 Myr old. The primary, HD 15407A (spectral type F5V), exhibitsstrong mid-infrared excess emission indicative of a recent catastrophiccollision between rocky planetary embryos or planets in its inner planetarysystem. Synthesis of all known stars with large quantities of dust in theirterrestrial planet zone indicates that for stars of roughly Solar mass thiswarm dust phenomenon occurs at ages between 30 and 100 Myr. In contrast, forstars of a few Solar masses, the dominant era of the final assembling of rockyplanets occurs earlier, between 10 and 30 Myr age. The incidence of the warmdust phenomenon, when compared against models for the formation of rockyterrestrial-like bodies, implies that rocky planet formation in the terrestrialplanet zone around Sun-like stars is common.

The Age of the HD 15407 System and the Epoch of Final Catastrophic Mass Accretion onto Terrestrial Planets around Sun-like Stars