Far-infrared spectrophotometry of oxygen-rich and S-type stars

Details Far-infrared spectrophotometry of oxygen-rich and S-type stars Far-infrared spectrophotometry of oxygen-rich and S-type stars

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999phdt.........4g&link_type=abstract

Thesis (PhD). THE UNIVERSITY OF CHICAGO, Source DAI-B 60/08, p. 4006, Feb 2000, 87 pages.

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Scientific paper

Airborne low-resolution 16-65 μm spectra of 19 oxygen-rich and 3 S stars, and simultaneous 100-200 μm photometry of the brightest objects are presented. The survey includes K and M giants, AGB stars, the post- AGB star AFGL 4106, and the hypergiant IRC+10420. Oxygen- rich stars with cold shells have emission bands at 24, 28, 33, 42, and 60 μm, caused by thermal emission from grains of crystalline silicates and water ice. Spectra of most supergiants and some giants are featureless at wavelengths greater than 20 μm, but supergiants with very high mass loss rates have very weak emission features from crystalline silicates. AGB stars with the 13 μm, feature have an emission feature centered at 29 μm. Weak, narrow emission features at 20.7, 22.4, 29.0, and 31.6 μm appear in some of the oxygen-rich stars. The shape of the 20 μm feature in VY CMa is variable. The S stars have a broader emission band that peaks near 30 μm. A simple model with several grain species is fitted to the spectrum of RX Boo. The 13 μm, feature probably arises from hot corundum grains. Other features can be fitted with combinations of amorphous and crystalline bronzite, olivine, clino-enstatite, and γ- Ca2SiO4. The calibration system, which is based on Mars, Uranus, and Callisto, is independent of ground-based photometric calibrations and the IRAS photometric calibration. Except for very bright objects, there is excellent agreement at 25 and 60 μm between this work and the IRAS Point Source Catalog.

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