The Distribution of Sio in the Circumstellar Envelope around Irc+10216

New interferometric observations of SiO J =5→ 4 circumstellar line emission around the carbon star IRC+10216, using the Submillimeter Array, are presented. Complemented by multi-transition single-dish observations, including infrared observations of ro-vibrational transitions, detailed radiative transfer modelling suggests that the fractional abundance of SiO in the inner part of the envelope, between ≈ 3–8 stellar radii, is as high as ≈ 1.5× 10. This is more than an order of magnitude higher than predicted by equilibrium stellar atmosphere chemistry in a carbon-rich environment and indicative of the importance of non-LTE chemical processes. In addition to the compact component, a spatially more extended (re ≈ 2.4× 10 16 cm) low-fractional-abundance (f0 ≈ 1.7× 10 ) region is required to fit the observations. This suggests that the majority of the SiO molecules are effectively accreted onto dust grains in the inner wind while the remaining gas-phase molecules are eventually photodissociated at larger distances. Evidence of departure from a smooth wind is found in the observed visibilities, indicative of density variations of a factor 2 to 5 on an angular scale corresponding to a time scale of about 200 years. Additionally, constraints on the velocity structure of the wind are obtained. Subject headings: stars: abundances – stars: AGB and post-AGB – stars: carbon – stars: circumstellar matter – stars: individual (IRC+10216) – stars: mass loss