Models for the temperature evolution of an asteroid with 150 km radius at different depth below the surface (from bottom to top: 5, 10, 15 km, and at centre) using different assumptions with respect to the heat conductivity. Left panel: homogeneous body. Solid line: constant heat conductivity K = 4.9 W m−1 K−1 and constantheat capacity cp = 865 J g−1. Dashed line: variation of heat conductivity with temperature T as W m−1 K−1 as typical for rock material (Xu et al. 2004), and variation of heat capacity as cp = 800 + 0.25 × T − 1.5 107∕T2 typical for H-chondrite material (Yomogida & Matsui 1984). Right panel: heterogeneous structure with compact core and a 2 km thick insulating mantle. Solid line: constant heat conductivity K = 4.9 W m−1 K−1 and constantheat capacity cp = 865 J g−1. Mantle with K reduced by a factor of 5, Dashed line: heat conductivity for H-chondrite material according to theheat conductivity model of this work and variation of heat capacity with T as for H-chondrite material. The time axis corresponds to age after formation. The body ist assumed to be formed at 2.2 Ma after CAI formation. The composition corresponds to that of H chondrites.
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