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Research over the past four decades has shown a rich variety of complexorganic molecular content in some meteorites. This current study is an attemptto gain a better insight into the thermal conditions experienced by thesemolecules inside meteorites during atmospheric entry. In particular, we wish tounderstand possible chemical processes that can occur during entry and thatmight have had an effect on complex organic or prebiotic species that weredelivered in this way to the early Earth. A simulation was written in Fortranto model heating by the shock generated during entry and the subsequent thermaldiffusion inside the body of a meteorite. Experimental data was used for thethermal parameters of several types of meteorites, including iron-nickel andseveral classes of chondrites. A Sutton-Graves model of stagnation-pointheating was used to calculate peak surface temperatures and an explicitdifference formula was used to generate thermal diffusion profiles for bothchondrites and iron-nickel type meteorites. Results from the simulation showpyrolytic temperature penetration to a depth of ca. 0.5 to 1 cm.Non-dissociative warming of meteorite interiors penetrates further to ca. 4 cm.These results support the findings that extraterrestrial delivery is a viableoption for prebiotic molecular "seeding" of a planet.

Thermally Induced Chemistry of Meteoritic Complex Organic Molecules: A New Heat-Diffusion Model for the Atmospheric Entry of Meteorites