2011A&A...534A...1D

We present new Herschel/PACS images at 70, 100, and 160µm of the well-known, nearby, carbon-rich asymptotic giant branch star IRC+10216 revealing multiple dust shells in its circumstellar envelope. For the first time, dust shells (or arcs) are detected until 320''. The almost spherical shells are non-concentric and have an angular extent between ∼40° and ∼200°. The shells have a typical width of 5''-8'', and the shell separation varies in the range of ∼10''-35'', corresponding to ∼500-1700yr. Local density variations within one arc are visible. The shell/intershell density contrast is typically ∼4, and the arcs contain some 50% more dust mass than the smooth envelope. The observed (nested) arcs record the mass-loss history over the past 16000yr, but Rayleigh-Taylor and Kelvin-Helmholtz instabilities in the turbulent astropause and astrosheath will erase any signature of the mass-loss history for at least the first 200000yr of mass loss. Accounting for the bowshock structure, the envelope mass around IRC+10216 contains >2M_☉ of gas and dust mass. It is argued that the origin of the shells is related to non-isotropic mass-loss events and clumpy dust formation.