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Only a few solar-type main sequence stars are known to be orbited by warmdust particles; the most extreme is the G0 field star BD+20 307 that emits ~4%of its energy at mid-infrared wavelengths. We report the identification of asimilarly dusty star HD 23514, an F6-type member of the Pleiades cluster. Astrong mid-IR silicate emission feature indicates the presence of small warmdust particles, but with the primary flux density peak at the non-standardwavelength of ~9 micron. The existence of so much dust within an AU or so ofthese stars is not easily accounted for given the very brief lifetime in orbitof small particles. The apparent absence of very hot (>~1000 K) dust at bothstars suggests the possible presence of a planet closer to the stars than thedust. The observed frequency of the BD+20 307/HD 23514 phenomenon indicatesthat the mass equivalent of Earth's Moon must be converted, via collisions ofmassive bodies, to tiny dust particles that find their way to the terrestrialplanet zone during the first few hundred million years of the life of many(most?) sun-like stars. Identification of these two dusty systems amongyouthful nearby solar-type stars suggests that terrestrial planet formation iscommon.

Warm dust in the terrestrial planet zone of a sun-like Pleiad: collisions between planetary embryos?