Long chain carbon molecules and diffuse interstellar lines

Abstract

An estimate of the abundances of chain hydrocarbon molecules expected in dense interstellar clouds as a result of gas-phase chemistry alone supports the hypothesis that the long chain molecules are responsible for the diffuse interstellar lines seen in the optical spectra of stars lying behind fairly low-density interstellar clouds. In particular, it is shown that the equilibrium abundances of the long chain carbon molecules may remain quite high even for molecules with as many as 11 carbon atoms.