Astronomy and Astrophysics – Astronomy
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...444..861s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 444, no. 2, p. 861-873
Astronomy and Astrophysics
Astronomy
33
Accretion Disks, Grain Size, Infrared Astronomy, Interstellar Matter, Main Sequence Stars, Abundance, Emission Spectra, Image Processing, Infrared Telescopes, Spatial Distribution, Spectrum Analysis
Scientific paper
We present multiwaveband observations of the K2 Vega-excess star SAO 26804 (= HD 233517). These include James Clerk Maxwell Telescope millimeter-wave photometry, plus spectra in the 8-13 microns and 18-24 microns atmospheric windows, an image at a wavelength of 10 microns through a broadband N filter and near-IR (JHKLL'M) photometry all taken at the United Kingdom Infrared Telescope. The source is resolved at 10 microns, and we can confirm with these observations that the IR excess seen in IRAS observations of this source is associated with the optical star. The image is consistent with the dust being confined to a disk with Full Width at Half Maximum (FWHM) 1.5 sec on the major axis, with an inclination angle of less than 30 deg away from edge-on. This represents the first confirmation that the dust in a Vega-excess star other than beta Pic is confined to a disk geometry. We present models of the source which show that many of the properties of the disk and the dust in it are similar to those which we have previously derived for the disk around SAO 179815, but that there are some very small grains in the disk around the star which give around SAO 179815, but that there are some very small grains in the disk around the star which give rise to a very prominent and narrow silicate dust feature at 9.7 microns and to so-called unidentified infrared bands in the 10 micron region. The larger grains are composed of a mixture of amorphous carbon and silicate with an abundance ratio consistent with an interstellar origin. The total mass of dust in the disk is 3.0 x 10-7 solar mass. Finally, our model suggests that there may be a substantial UV and/or soft X-ray flux from SAO 26804, consistent with it being a very young and rather active star.
Arens John F.
Barlow Michael J.
Graham James R.
Jernigan Garret J.
Keto Eric
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