Journal
ASTRONOMY & ASTROPHYSICS
Volume 534, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201117360
Keywords
stars: AGB and post-AGB; circumstellar matter; stars: carbon; stars: individual: IRC+10216
Categories
Funding
- BMVIT (Austria)
- ESA-PRODEX (Belgium)
- CEA/CNES (France)
- DLR (Germany)
- ASI (Italy)
- CICT/MCT (Spain)
- Fund for Scientific Research Flanders (FWO)
- Belgian Federal Science Policy Office
- ESA
- Austrian Science Fund FWF [P23586-N16, I163-N16]
- STFC [ST/G002827/1] Funding Source: UKRI
- Austrian Science Fund (FWF) [P 23586] Funding Source: researchfish
- Science and Technology Facilities Council [ST/G002827/1] Funding Source: researchfish
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We present new Herschel/PACS images at 70, 100, and 160 mu m 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 similar to 40 degrees and similar to 200 degrees. The shells have a typical width of 5 ''-8 '' and the shell separation varies in the range of similar to 10 ''-35 '',corresponding to similar to 500-1 700 yr. Local density variations within one arc are visible. The shell/intershell density contrast is typically similar to 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 16 000 yr, 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 200 000 yr of mass loss. Accounting for the bowshock structure, the envelope mass around IRC+10216 contains >2 M-circle dot 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.
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