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We hypothesise that differences in the temperatures at which the rockymaterial condensed out of the nebula gas can lead to differences in thecomposition of key rocky species (e.g., Fe, Mg, Si, Ca, Al, Na) and thus planetbulk density. Such differences in the observed bulk density of planets mayoccur as a function of radial location and time of planet formation. In thiswork we show that the predicted differences are on the cusp of being detectablewith current instrumentation. In fact, for HD 219134, the 10 % lower bulkdensity of planet b compared to planet c could be explained by enhancements inCa, Al rich minerals. However, we also show that the 11 % uncertainties on theindividual bulk densities are not sufficiently accurate to exclude the absenceof a density difference as well as differences in volatile layers. Besides HD219134 b, we demonstrate that 55 Cnc e and WASP-47 e are similar candidates ofa new Super-Earth class that have no core and are rich in Ca and Al mineralswhich are among the first solids that condense from a cooling proto-planetarydisc. Planets of this class have densities 10-20% lower than Earth-likecompositions and may have very different interior dynamics, outgassinghistories and magnetic fields compared to the majority of Super-Earths.

A new class of Super-Earths formed from high-temperature condensates: HD219134 b, 55 Cnc e, WASP-47 e