Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...348l..55y&link_type=abstract
Astronomy and Astrophysics, v.348, p.L55-L58 (1999)
Astronomy and Astrophysics
Astrophysics
51
Stars: Agb And Post-Agb, Stars: Atmospheres, Stars: Late-Type, Infrared: Stars
Scientific paper
The ISO/SWS spectrum of o Cet taken at its maximum exhibits an absorption-like feature between 3.5 and 4.0 mu m. We present evidence that the feature is due to emission of H_2O and SiO molecules, in a layer extended to about two stellar radii with an excitation temperature of 2000 K. These hot molecules are also observed in a spectrum of Z Cas near minimum, but this time in absorption. A simple plane-parallel model is used to fit the spectra of these two stars. The H_2O column densities and excitation temperatures in the layers are found to be similar in both stars. The difference of the H_2O band is thus primarily due to the layer size. The H_2O layers seem to be more extended at visual maximum, probably related to the stellar pulsation. The estimated lower limit to the local gas density in the layers of ~ 10(11) cm(-3) is in good agreement with theoretical predictions from dynamical model atmospheres. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) with the participation of ISAS and NASA. The SWS is a joint project of SRON and MPE.
Cami Jan
de Jong Teije
Yamamura Issei
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