Molecular line spectra from circumstellar envelopes. I - Excitation of (C-12)O, (C-13)O, and CS, and the formation of line profiles

Details Molecular line spectra from circumstellar envelopes. I - Excitation of (C-12)O, (C-13)O, and CS, and the formation of line profiles Molecular line spectra from circumstellar envelopes. I - Excitation of (C-12)O, (C-13)O, and CS, and the formation of line profiles

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...195..198s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 195, no. 1-2, April 1988, p. 198-207.

Astronomy and Astrophysics

Astrophysics

23

Cool Stars, Line Spectra, Molecular Spectra, Stellar Envelopes, Supergiant Stars, Carbon Monoxide, Emission Spectra, Radiative Transfer, Stellar Winds, Sulfides

Scientific paper

The excitation mechanisms of (C-12)O, (C-13)O, and CS were investigated in the mass-loss range between 0.000001 and 0.0001 solar mass/yr, performing radiative transfer calculations for molecular emission lines formed in the winds of cool giants and supergiants. These calculations included excitation of collisions with H2 as well as scattering of IR and microwave radiation emergent from warm dust particles, from the stellar photosphere, and the cosmic background radiation. It was found that, for (C-12)O molecules, there are three distinct regions of mass loss: an LTE region for the mass accretion rate greater than about 0.00003 solar mass/yr, where the (C-12)O molecules are nearly exclusively excited by collisions; an NLTE region for the mass accretion rate between 0.000003 and 0.00003 solar mass/yr; and a maser region for the mass accretion rate less than 0.000003 solar mass/yr. For (C-13)O and CS, no LTE region is present and masers appear at rather large mass loss rates. The line formation processes are discussed in detail.

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