Images of low excitation HC_3_N emission from IRC+10 216.

Details Images of low excitation HC_3_N emission from IRC+10 216. Images of low excitation HC_3_N emission from IRC+10 216.

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...290..198w&link_type=abstract

Astronomy and Astrophysics 290, 198-206 (1994)

Astronomy and Astrophysics

Astrophysics

5

Stars: Circumstellar Matter, Stars: Individual (Irc+10 216), Molecular Processes, Radio Lines: Stars

Scientific paper

Spatially and kinematically resolved images of emission in the ground state J=1->0 F=2->1 line of HC_3_N at λ=3.3cm are presented which illustrate the structure of the molecular shell surrounding the evolved carbon star IRC+10 216. This ground state line, which traces cool material, should provide a good probe of outlying material. The emission appears ringlike, peaking at a radial distance of 12", but with substantial contributions from the entire envelope, extending to a radial distance of about 30" from the star. The J=1->0 F=2->1 line emission in the vibrationally excited 2ν_7_^2^ state has not been detected. A model is developed which reproduces both the images shown here, and also other images from lines in the millimeter wavelength region. The results show that the ringlike appearance of HC_3_N emission occurs because of the shell form of HC_3_N abundance distribution, with a peak at radius 15" falling off more slowly exterior to the peak than interior to it. A second model produces a better fit to the observations, but requires an interior region of unrealistically high HC_3_N abundance and a low mass loss rate.

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