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The field of extrasolar planets has rapidly expanded to include the detectionof planets with masses smaller than that of Uranus. Many of these are expectedto have little or no hydrogen and helium gas and we might find Earth analogsamong them. In this paper we describe our detailed interior models for a richvariety of such massive terrestrial and ocean planets in the 1-to-10 earth-massrange (super-Earths). The grid presented here allows the characterization ofthe bulk composition of super-Earths detected in transit and with a measuredmass. We show that, on average, planet radius measurements to better than 5%,combined with mass measurements to better than 10% would permit us todistinguish between an icy or rocky composition. This is due to the fact thatthere is a maximum radius a rocky terrestrial planet may achieve for a givenmass. Any value of the radius above this maximum terrestrial radius impliesthat the planet contains a large (> 10%) amount of water (ocean planet).

Detailed Models of super-Earths: How well can we infer bulk properties?