Molecular absorption and emission in W Hya

Details Molecular absorption and emission in W Hya Molecular absorption and emission in W Hya

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..349j&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 349

Physics

1

W Hydra, Water Vapour

Scientific paper

We obtained SWS full grating scans of the semi-regular variable star W Hya which show a multitude of molecular absorption bands in the near infrared. The high resolution spectrum makes it possible to identify the responsible species as H2O, OH, CO, CO2 and SiO. Most of the absorption seems to arise from a layer close to the star. There is an evidence for cooler gas farther out in the circumstellar envelope as well. W Hya also shows CO2 bands in its mid-IR spectrum. We have obtained Fabry-Perot spectra centred on these ro-vibrational bands. A preliminary estimate of the temperature of emission lines superimposed on the absorption of the fundamental (0110-0000) band is about 270 K, although the overall absorption of this band indicates a higher temperature, and possibly contribution from higher vibrational transitions which fall in the same wavelength region. Results from CO and OH modelling support the idea that there is a hot layer of CO2 close to the star.

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