Other
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9305w&link_type=abstract
American Astronomical Society, AAS Meeting #211, #93.05; Bulletin of the American Astronomical Society, Vol. 39, p.890
Other
1
Scientific paper
Oxygen-rich Asymptotic Giant Branch (AGB) stars return a significant amount of material to the interstellar medium, from which new stars and planets form.
The dust around AGB stars are studied by means of infrared spectroscopy, and their spectral features can be broadly classified into eight classes according to the ratios of fluxes at 10, 11 and 12um. Furthermore, these Silicate Emission (SE) classes can be subdivided according to whether the spectrum exhibits an enigmatic 13 um feature, whose carrier remains unknown. In addition, other features in the 15-20 um range appear to correlate with the 13 um feature. Using the radiative transfer code, DUSTY, we manipulate the parameters of circumstellar dust shells; which include star temperature, dust condensation temperature, optical depth, density distribution, shell thickness, and composition via optical constants to produce synthetic spectrum and match observations. In particular, we focus on the contribution of magnesium-iron oxides to the 15-20μm range that has emission. We present preliminary results for the mineralogy of 13um O-rich AGB stars. SE 1 is dominated by amorphous alumina features and the SE 6 is dominated by silicate features but both carry a narrow 9.7um feature that cannot be explained with the optical constants for amorphous silicates. Furthermore, this feature is not restricted the 13um objects and thus is unrelated to its carrier.
Speck Angela Karen
Wheeler Caleb
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