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Some observations of warm carbon chain chemistry (WCCC) cores indicate thatthey are often located near the edges of molecular clouds. This finding maysuggest that WCCC is promoted in star-forming cores exposed to radiation fromthe interstellar medium. We aim to investigate the chemistry of carbon chainsin such a core. A chemical simulation of a gas parcel in a low-massstar-forming core with a full level of irradiation by interstellar photons andcosmic rays was compared to a simulation of a core receiving only one-tenth ofsuch irradiation. In the full irradiation model, the abundances of carbonchains were found to be higher by a factor of few to few hundred, compared tothe model with low irradiation. Higher carbon-chain abundances in theprestellar stage and, presumably, in the extended circumstellar envelope, arisebecause of irradiation of gas and dust by interstellar photons and cosmic rays.A full standard rate of cosmic-ray induced ionization is essential for a highcarbon-chain abundance peak to occur in the circumstellar envelope, which isheated by the protostar (the "true" WCCC phenomenon). The full irradiationmodel has lower abundances of complex organic molecules than thelow-irradiation model. We conclude that WCCC can be caused by exposure of astar-forming core to interstellar radiation, or even just to cosmic rays. TheAppendix describes an updated accurate approach for calculating the rate ofcosmic-ray induced desorption.

The connection between warm carbon chain chemistry and interstellar irradiation of star-forming cores