Growth of carbon chains in IRC +10216 mapped with ALMA^⋆,⋆⋆

¹ Instituto de Ciencia de Materiales de Madrid, CSIC, C/ Sor Juana Inés de la Cruz 3, 28049 Cantoblanco, Spain
e-mail: marcelino.agundez@icmm.csic.es
² Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 St.-Martin-d’Hères, France
³ Université de Toulouse, UPS-OMS, IRAP, 31000 Toulouse, France
⁴ CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
⁵ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
⁶ School of Engineering and Applied Sciences, Harvard University, Cambridge, MA 02138, USA

Received: 17 December 2016
Accepted: 13 February 2017

Abstract

Linear carbon chains are common in various types of astronomical molecular sources. Possible formation mechanisms involve both bottom-up and top-down routes. We have carried out a combined observational and modeling study of the formation of carbon chains in the C-star envelope IRC +10216, where the polymerization of acetylene and hydrogen cyanide induced by ultraviolet photons can drive the formation of linear carbon chains of increasing length. We have used ALMA to map the emission of λ 3 mm rotational lines of the hydrocarbon radicals C₂H, C₄H, and C₆H, and the CN-containing species CN, C₃N, HC₃N, and HC₅N with an angular resolution of ~1′′. The spatial distribution of all these species is a hollow 5–10′′ wide spherical shell located at a radius of 10–20′′ from the star, with no appreciable emission close to the star. Our observations resolve the broad shell of carbon chains into thinner subshells that are 1–2′′ wide and not fully concentric, indicating that the mass-loss process has been discontinuous and not fully isotropic. The radial distributions of the species mapped reveal subtle differences: while the hydrocarbon radicals have very similar radial distributions, the CN-containing species show more diverse distributions, with HC₃N appearing earlier in the expansion and the radical CN extending later than the rest of the species. The observed morphology can be rationalized by a chemical model in which the growth of polyynes is mainly produced by rapid gas-phase chemical reactions of C₂H and C₄H radicals with unsaturated hydrocarbons, while cyanopolyynes are mainly formed from polyynes in gas-phase reactions with CN and C₃N radicals.