The dust around the carbon star IRC +10216

Details The dust around the carbon star IRC +10216 The dust around the carbon star IRC +10216

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..647j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 267, April 15, 1983, p. 647-652. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

56

Carbon Stars, Cosmic Dust, Infrared Stars, Interstellar Matter, Stellar Envelopes, Hydrocyanic Acid, Interstellar Extinction, Opacity, Stellar Mass Ejection, Ultraviolet Radiation

Scientific paper

Mass loss from late-type stars is important both in the evolution of these objects and for replenishment of the interstellar medium with processed material. Because the outflows are cool and dense, grains form. The present investigation is concerned with the nature of the extinction of the grains in the carbon star IRC+10216. The basic method employed involves the study of the extinction as a function of wavelength around IRC+10216. By a comparison with different models, it is then possible to infer which grain model is more likely to be correct. It is concluded that the dust around IRC+10216 is composed of relatively small grains. The grains are either amorphous carbon or graphite similar to that described by Mezger et al. (1982), but not like the graphite described by Mitchell and Robinson (1980). In particular, the grains around IRC + 10216 are relatively efficient emitters in the infrared. If this result is true of carbon stars in general, it means that the carbon grains present in the interstellar medium are much cooler than often believed.

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