Observations and modelling of spectral energy distributions of carbon stars with optically thin envelopes

Details Observations and modelling of spectral energy distributions of carbon stars with optically thin envelopes Observations and modelling of spectral energy distributions of carbon stars with optically thin envelopes

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.296..545b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 296, Issue 3, pp. 545-563.

Astronomy and Astrophysics

Astronomy

8

Stars: Carbon, Circumstellar Matter

Scientific paper

We present broad-band photometry in the optical, near-infrared and submillimetre, and mid-infrared spectrophotometry of a selection of carbon stars with optically thin envelopes. Most of the observations were carried out simultaneously. Beside the emission feature at 11.3mum due to silicon carbide grains in the circumstellar environment, many of our mid-infrared spectra show an emission feature at 8.6mum. All the observed spectral energy distributions exhibit a very large far-infrared flux excess. Both these features are indeed common to many carbon stars surrounded by optically thin envelopes. We have modelled the observed spectral energy distributions by means of a full radiative transfer treatment, paying particular attention to the features quoted above. The peak at 8.6mum is usually ascribed to the presence of hydrogenated amorphous carbon grains. We find also that the feature at 8.6mum might be reproduced by assuming that the stars have a circumstellar environment formed of both carbon- and oxygen-rich dust grains, although this is in contrast with what one should expect in a carbon-rich environment. The far-infrared flux excess is usually explained by the presence of a cool detached dust shell. Following this hypothesis, our models suggest a time-scale for the modulation of the mass-loss rate of the order of some 10^3yr.

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