CO 4.6 micron emission lines from the IRC +10216 inner envelope

Details CO 4.6 micron emission lines from the IRC +10216 inner envelope CO 4.6 micron emission lines from the IRC +10216 inner envelope

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299..424s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 424-442. Research supported by the Robert A. Welch Fo

Astronomy and Astrophysics

Astronomy

23

Carbon Monoxide, Infrared Astronomy, Infrared Stars, Stellar Envelopes, Stellar Mass Ejection, Emission Spectra, Line Spectra, Molecular Spectra, Optical Thickness, Radiative Transfer, Spectrum Analysis

Scientific paper

The authors present the results of an investigation of gas in the inner envelope of IRC +10216 at a scale size (≡2arcsec) never observed previously. Observations were made at the 4.6 μm fundamental vibration-rotation band of CO, employing an annular observing aperture to isolate radiation resonantly scattered from the extended molecular envelope. Both CO and 13CO show evidence of high-velocity features in the blue wing of the line, beyond the 15 km s-1 expansion velocity. In order to derive physical quantities from the many P and R branch lines present in the infrared spectra, the authors develop an analytical model to calculate the excitation of these lines due to thermal emission from dust. The lines are optically thick, and trapping of line radiation has been included. The observations show that the kinetic temperature at radius r = 2arcsec is ≡180 - 225K. A mass loss rate for the inner envelope of ≡(5-7)×10-5M_sun;yr-1 is derived.

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