The Conductive Cooling of Planetesimals With Temperature‐Dependent Properties

Modeling the planetary heat transport of small bodies in early Solar System allows us to understand geological context meteorite samples. Conductive cooling planetesimals is controlled by thermal conductivity, capacity, and density, which are functions temperature (T). We investigate if incorporation T-dependence properties introduction a nonlinear term equation could result different interpretations origin classes meteorites. have developed finite difference code perform numerical models conductively planetesimal with T-dependent find that including produces considerable differences history, turn estimated timing depth genesis. interrogate effects varying input parameters this model explore conductivity simple linear functions. Then we apply non-monotonic for density fitted published experimental data. For representative calculation 250 km radius pallasite parent body, delay onset core crystallization dynamo activity ∼40 Myr, approximately equivalent increasing 10%, extend ∼3 Myr. This affects range radii sizes body compatible paleomagnetic evidence. approach can also be used T-evolution other differentiated minor planets primitive constrain formation associated