The role of CO 67 - 186 μm lines in astrophysics.

Details The role of CO 67 - 186 μm lines in astrophysics. The role of CO 67 - 186 μm lines in astrophysics.

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999acasn..40..376m&link_type=abstract

Acta Astron. Sin., Vol. 40, No. 4, p. 376 - 381

Other

Carbon Monoxide: Line Formation, Carbon Monoxide: Planetary Nebulae, Carbon Monoxide: Protoplanetary Nebulae, Carbon Monoxide: Circumstellar Shells

Scientific paper

A spherical and large-velocity-gradient model is adopted for the theoretical calculations of NGC 7027, AFGL 2688 and IRC +10216, whose emissions of CO far-infrared lines are comparatively strong. The statistical equilibrium calcualtions cover 107 energy levels. The CO far-infrared lines of IRC +10216 are excited mainly by the central star, while for NGC 7027 and AFGL 2688 by the shocked warm and dense gases. The excitation mechanism is also discussed for other observed objects by using ISO. The CO spectra in the wavelength range 67 - 186 μm are important probes for detecting the objects with kinetic temperatures of several hundred degrees, i.e. the envelopes of carbon or oxygen-rich stars, planetary nebulae, young stellar objects and star-forming complexes.

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