Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.286.1003d&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 286, Issue 4, pp. 1003-1011.
Astronomy and Astrophysics
Astronomy
3
Stars: Carbon, Circumstellar Matter, Stars: Evolution, Stars: Individual: Irc +10216, Stars: Mass-Loss, Radio Lines: General
Scientific paper
We construct a simple model for the emission-line profiles of CO from the circumstellar envelope (CSE) of the carbon-rich star IRC +10216. Using the Sobolev approximation, and a given gas temperature distribution (gTD) we construct simulated observations of this source. We find that the `canonical' gTD [T(r)~r^-0.7] cannot reproduce the observations. Guided by a strong correlation between telescope beamsize and peak intensity, we vary the gTD to fit the observations, and find that the data are best reproduced by T(r)~r^-1. This power law is consistent with CO line radiation being the dominant coolant in the CSE. Differences between this and other results may be the result of a previous lack of high-resolution observations, the use of older CO collisional rates, or reduced mass-loss rate. Although an assumed source distance of 150 pc gives the best fit to the data, we cannot rule out the possibility of a larger source distance (e.g. 300 pc).
Doty Steven D.
Leung Chun Ming
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