The chemistry of extragalactic carbon stars

TL;DR

This study models the circumstellar chemistry of extragalactic carbon stars in low-metallicity environments, revealing higher hydrocarbon abundances and suppressed oxygen and nitrogen chemistry, with predictions for detectable molecular emissions.

Contribution

It provides the first detailed chemical models of extragalactic carbon stars in low-metallicity environments, linking observations with molecular abundance predictions.

Findings

Acetylene is more abundant than CO in low-metallicity carbon stars.

Larger hydrocarbons have higher abundances at Magellanic Cloud metallicities.

Several molecules are predicted to be detectable with ALMA.

Abstract

Prompted by the ongoing interest in Spitzer Infrared Spectrometer spectra of carbon stars in the Large Magellanic Cloud, we have investigated the circumstellar chemistry of carbon stars in low-metallicity environments. Consistent with observations, our models show that acetylene is particularly abundant in the inner regions of low metallicity carbon-rich AGB stars -- more abundant than carbon monoxide. As a consequence, larger hydrocarbons have higher abundances at the metallicities of the Magellanic Clouds than in stars with solar metallicity. We also find the oxygen and nitrogen chemistry is suppressed at lower metallicity, as expected. Finally, we calculate molecular line emission from carbon stars in the Large and Small Magellanic Cloud and find that several molecules should be readily detectable with the Atacama Large Millimeter Array at Full Science operations.