Crystallinity versus mass-loss rate in AGB stars

Details Crystallinity versus mass-loss rate in AGB stars Crystallinity versus mass-loss rate in AGB stars

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000esasp.456..199k&link_type=abstract

ISO beyond the peaks: The 2nd ISO workshop on analytical spectroscopy. Eds. A. Salama, M.F.Kessler, K. Leech & B. Schulz. ESA-SP

Physics

1

Iso, Stars: Agb Stars, Models: Radiative Transfer, Dust: Crystalline And Amorphous Silicates

Scientific paper

Observational studies have shown that O-rich AGB stars exhibit crystalline silicate features in their spectra only if their mass loss rate is higher than a certain threshold value. Usually, this is interpreted as evidence that crystalline silicates are not present in the dust shells of low mass-loss rate objects. In this study, model calculations have been performed to provide an alternative explanation to the lack of crystalline silicate features in the spectrum of low mass-loss rate AGB stars. The absence of discernible crystalline silicate features is here attributed to the extremely low Fe-content of crystalline silicate, rather than the absence of crystalline silicates. As a result, the crystalline grains do not absorb much stellar light (in the 1-3 μm range), and the crystalline features only become apparent when the peak of the spectral energy distribution has shifted to the 10-20 μm range where crystalline silicates possess strong resonances.

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