Thermal and maser molecular lines from the envelope of IRC + 10216

Details Thermal and maser molecular lines from the envelope of IRC + 10216 Thermal and maser molecular lines from the envelope of IRC + 10216

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...286..276n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 1, 1984, p. 276-283.

Astronomy and Astrophysics

Astrophysics

52

Infrared Stars, Masers, Molecular Spectra, Stellar Envelopes, Stellar Spectra, Abundance, Carbon Monoxide, Molecular Excitation, Silicon Oxides, Stellar Mass Ejection, Stellar Models

Scientific paper

A theoretical model of the circumstellar shell of IRC + 10216 is developed based on the high-sensitivity spectra of the diatomic molecules SiS, SiO, CO-12 and CO-13. Asymmetry observed in the line profiles of the molecules is explained quantitatively in terms of the absorption of the emission from the warm internal region of the shell by the cold external layers. Most of the molecular emission regions are confined within a radius smaller than about 2 x 10 to the 17th cm. The model shows that all molecular features are thermally excited except for the SiS line emission at v = 0, J = 1-0 transition, which exhibits a maser spike close to the infrared core of IRC + 10216. The narrow blueshifted feature at -40 km/s is due to the amplification of the radiation emitted by the core, whereas the broad underlying blueshifted component at -40 km/s and the redshifted wings at -13 km/s correspond to the overall maser emission throughout the envelope. It is suggested on the basis of the theoretical calculations that an increase in the number of infrared photons produced by the central heating sources (the 600 K core and the 375 K) dust component tends to enhance the overall intensity of the SiS, SiO and CO-13 spectra.

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