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A high fraction of carbon bound in solid carbonaceous material is observed toexist in bodies formed in the cold outskirts of the solar nebula, while bodiesin the terrestrial planets region contain nearly none. We study the fate of thecarbonaceous material during the spiral-in of matter as the sun accretes matterfrom the solar nebula. From observational data on the composition of the dustcomponent in comets and interplanetary dust particles, and from data onpyrolysis experiments, we construct a model for the composition of the pristinecarbonaceous material in the outer parts of the solar nebula. We study thepyrolysis of the refractory and volatile organic component and the concomitantrelease of high-molecular-weight hydrocarbons under quiescent conditions ofdisk evolution where matter migrates inwards. We also study the decompositionand oxidation of the carbonaceous material during violent flash heating events,which are thought to be responsible for the formation of chondrules. It isfound that the complex hydrocarbon components are removed from the solid diskmatter at temperatures between 250 and 400 K, while the amorphous carboncomponent survives up to 1200 K. Without efficient carbon destruction duringflash-heating associated with chondrule formation the carbon abundance ofterrestrial planets, except for Mercury, would be not as low as it is found incosmochemical studies. Chondrule formation seems to be a process that iscrucial for the carbon-poor composition of the material of terrestrial planets.

The spatial distribution of carbon dust in the early solar nebula and the carbon content of planetesimals