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The Infrared Spectrograph on the Spitzer Space Telescope observed 184 carbonstars in the Magellanic Clouds. This sample reveals that the dust-productionrate (DPR) from carbon stars generally increases with the pulsation period ofthe star. The composition of the dust grains follows two condensationsequences, with more SiC condensing before amorphous carbon in metal-richstars, and the order reversed in metal-poor stars. MgS dust condenses inoptically thicker dust shells, and its condensation is delayed in moremetal-poor stars. Metal-poor carbon stars also tend to have stronger absorptionfrom C2H2 at 7.5 um. The relation between DPR and pulsation period showssignificant apparent scatter, which results from the initial mass of the star,with more massive stars occupying a sequence parallel to lower-mass stars, butshifted to longer periods. Accounting for differences in the mass distributionbetween the carbon stars observed in the Small and Large Magellanic Cloudsreveals a hint of a subtle decrease in the DPR at lower metallicities, but itis not statistically significant. The most deeply embedded carbon stars havelower variability amplitudes and show SiC in absorption. In some cases theyhave bluer colors at shorter wavelengths, suggesting that the central star isbecoming visible. These deeply embedded stars may be evolving off of the AGBand/or they may have non-spherical dust geometries.

The infrared spectral properties of Magellanic carbon stars