Circumstellar silicon chemistry and the SiO maser

Details Circumstellar silicon chemistry and the SiO maser Circumstellar silicon chemistry and the SiO maser

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.203..125c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 203, Apr. 1983, p. 125-146. Research supported by the Nederlandse Organ

Astronomy and Astrophysics

Astronomy

43

Cosmochemistry, Masers, Red Giant Stars, Silicon Oxides, Stellar Envelopes, Ultraviolet Radiation, Carbon Monoxide, Hydrogen, Photoabsorption, Photodissociation, Reaction Kinetics, Silicates

Scientific paper

The authors have investigated the effects of stellar chromospheric UV radiation on the composition of gaseous layers around O-rich red-giant stars losing mass, with particular attention to the almost static layers recently identified from infrared spectra. The UV radiation can strongly inhibit molecular association. Si-chemistry is studied in the steady-state approximation, and some simple results concerning time-scales, shell optical depths and photoelectric heating rates are deduced. Around α Orionis the authors predict that CO should be fully associated but that hydrogen should be in atomic form. They show that a chemical pump for SiO masers would operate too slowly to explain the observed photon emission rate, and propose some observational diagnostics of circumstellar molecular processes.

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