Abstract
Recently observed systematic trends of asteroidal composition with respect to size and heliocentric distance are interpreted according to the hypothesis that primordial asteroidal thermal evolution was driven by electromagnetic induction in a dense pre-main-sequence solar wind. It is found that the spatial distribution of induction heating corresponds well with that inferred from the present-day distribution of asteroidal compositional types when reasonable proto-Solar-System characteristics are assumed. From this match is deduced a rough constraint on the induction heating epoch's duration (≈10 5years) and the temperature-dependent electrical conductivity of the protoasteroidal material (about the same as that of the C2 meteorite Murcheson).
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