Is SiO observed in the uv spectrum of Beta Gem?

Details Is SiO observed in the uv spectrum of Beta Gem? Is SiO observed in the uv spectrum of Beta Gem?

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8294j&link_type=abstract

HST Proposal ID #8294

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Hst Proposal Id #8294 Cool Stars

Scientific paper

Beta Gem {HD 62509} is a K0 III star with relatively low ultraviolet {uv} emission line fluxes and X-ray emission, and is thought to be a helium core- burning `clump' giant. However, since it lies at a distance of only about 10 parsecs the fluxes at the Earth are sufficient for detailed spectral studies in the uv. Although our main interest in the star has been in modelling for the purposes of establishing and understanding the energy balance requirements, this proposal is concerned with a specific aspect of its spectrum around 2320 Angstrom to 2365 Angstrom. In Beta Gem {HD 62509} and cooler giants the strongest lines in this region are those of C II, Si II and Fe II. The spectrum of Beta Gem {HD 62509} is so far unique in that it also shows a number of narrow emission features that are not observed in the cooler stars, with an overall structure that suggests the presence of a molecular band. We wish to investigate the possibility that this is the A^1Pi - X^1Sigma {0 - 0} b an d of SiO, which has never been identified in an astrophysical spectrum. This requires the high spectral resolution of STIS. Other bands in the above system would then also be expected in the region from about 2300 Angstrom to 2500 Angstrom. Chromospheric models would be used to understand the presence of the SiO band system in Beta Gem {HD 62509} and its absence in cooler giants.

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