Volume 382, Number 1, JanuaryIV 2002
|Page(s)||222 - 240|
|Published online||15 January 2002|
Crystalline silicate dust around evolved stars *
II. The crystalline silicate complexes
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2 School of Materials Science and Engineering, Georgia Tech, Atlanta, GA 30332-0245, USA
3 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium
4 SRON Laboratory for Space Research Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
Corresponding author: F. J. Molster, firstname.lastname@example.org
Accepted: 5 November 2001
This is the second paper in a series of three in which we present an exhaustive inventory of the solid state emission bands observed in a sample of 17 oxygen-rich dust shells surrounding evolved stars. The data were taken with the Short and Long Wavelength Spectrographs on board of the Infrared Space Observatory (ISO) and cover the 2 to 200 μm wavelength range. Apart from the broad 10 and 18 μm bands that can be attributed to amorphous silicates, at least 49 narrow bands are found whose position and width indicate they can be attributed to crystalline silicates. Most of these emission bands are concentrated in well defined spectral regions (called complexes). We define 7 of these complexes; the 10, 18, 23, 28, 33, 40 and 60 micron complex. We derive average properties of the individual bands. Almost all of these bands were not known before ISO. Comparison with laboratory data suggests that both olivines (MgFeSiO4) and pyroxenes (MgxFeSiO3) are present, with x close to 1, i.e. the minerals are very Mg-rich and Fe-poor. This composition is similar to that seen in disks surrounding young stars and in the solar system comet Hale-Bopp. A significant fraction of the emission bands cannot be identified with either olivines or pyroxenes. Possible other materials that may be the carriers of these unidentified bands are briefly discussed. There is a natural division into objects that show a disk-like geometry (strong crystalline silicate bands), and objects whose dust shell is characteristic of an outflow (weak crystalline silicate bands). In particular, stars with the 33.5 μm olivine band stronger than about 25 percent over continuum are invariably disk sources. Likewise, the 60 μm region is dominated by crystalline silicates in the disk sources, while it is dominated by crystalline H2O ice in the outflow sources. We show that the disk and outflow sources have significant differences in the shape of the emission bands. This difference must be related to the composition or grain shapes of the dust particles. The incredible richness of the crystalline silicate spectra observed by ISO allows detailed studies of the mineralogy of these dust shells, and is the origin and history of the dust.
Key words: infrared: stars / circumstellar matter / stars: AGB and post-AGB; mass loss / Planetary Nebulae: general / dust, extinction
© ESO, 2002
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