IR fluxes and photometry of oxygen-rich stars (Le Sidaner+ 1996)

Details IR fluxes and photometry of oxygen-rich stars (Le Sidaner+ 1996) IR fluxes and photometry of oxygen-rich stars (Le Sidaner+ 1996)

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..33140896l&link_type=abstract

VizieR On-line Data Catalog: J/A+A/314/896. Originally published in: 1996A&A...314..896L

Physics

Stars: Giant, Photometry: Ubvri

Scientific paper

We present mid-infrared (10-20μm) photometry obtained on 27 variable oxygen-rich late-type stars, at different epochs during the period 1984-1990. The sample includes representative objects of Miras with optical counterparts, as well as type II OH/IR sources; there are also at least 2 supergiants. These measurements are merged with near-infrared ones, already reported and obtained quasi-simultaneously, to derive 72 (1-20μm) broad band energy distributions. These results are complemented also with IRAS data and flux measurements obtained in the sub-millimeter range. The resulting spectra are interpreted in terms of a circumstellar dust shell radiative transfer model applied for each object at different phases of their lightcurves. The modelling appears to be consistent for a large variety of oxygen-rich sources with optical depth at 10μm ranging from ~0.01 to 10. The temperature of formation of the grains is taken to range from 800 to 950K depending on the pressure at the site of dust formation (P~10-7-10-4dyn.cm-2). Physical parameters such as inner radius of the circumstellar dust shell, bolometric luminosity and mass-loss rate are evaluated. For the objects in the sample, the mass-loss rate ranges from 2x10-8 to 10-4M&sun;/yr. In the context of the planned and underway near-infrared surveys we discuss the relations between color indices and optical depth for oxygen-rich sources. Circumstellar shell optical depths and mass-loss rates are shown to be correlated to the [K-12μm] color. Unfortunately, near-infrared data alone seem to be insufficient to determine physical parameters reliably. For a description of the UBVRI photometric systems, see e.g. (7 data files).

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