Molecular abundances in IRC + 10216

Details Molecular abundances in IRC + 10216 Molecular abundances in IRC + 10216

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.281..263m&link_type=abstract

Nature, vol. 281, Sept. 27, 1979, p. 263-266. Research supported by the Robert A. Welch Foundation.

Computer Science

103

Abundance, Carbon Stars, Infrared Stars, Stellar Atmospheres, Chemical Composition, Chemical Equilibrium, Gas Pressure, Grains, Graphite, Interplanetary Dust, Optical Thickness, Pressure Effects, Silicon Carbides, Silicon Oxides, Temperature Distribution

Scientific paper

The observed molecular column densities in IRC + 10216 can be matched by chemical equilibrium calculations for a temperature approximately equal to 1,250 K, pressure approximately equal to 100 dynes/sq cm, and no graphite grain formation. Condensation of silicon carbide into grains may explain the low observed abundances of SiO and SiS. A compressed gaseous shell may be formed between successive dust shells lost by the central variable carbon star during each of its cycles

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