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• W3103946412 abstract "<i>Aims. <i/>We present a diagnostic tool to determine the abundance of the crystalline silicate forsterite in AGB stars surrounded by a thick shell of silicate dust. Using six infrared spectra of high mass-loss oxygen rich AGB stars we obtain the forsterite abundance of their dust shells.<i>Methods. <i/>We use a monte carlo radiative transfer code to calculate infrared spectra of dust enshrouded AGB stars. We vary the dust composition, mass-loss rate and outer radius. We focus on the strength of the 11.3 and the 33.6 <i>μ<i/>m forsterite bands, that probe the most recent (11.3 <i>μ<i/>m) and older (33.6 <i>μ<i/>m) mass-loss history of the star. Simple diagnostic diagrams are derived, allowing direct comparison to observed band strengths.<i>Results. <i/>Our analysis shows that the 11.3 <i>μ<i/>m forsterite band is a robust indicator for the forsterite abundance of the current mass-loss period for AGB stars with an optically thick dust shell. The 33.6 <i>μ<i/>m band of forsterite is sensitive to changes in the density and the geometry of the emitting dust shell, and so a less robust indicator. Applying our method to six high mass-loss rate AGB stars shows that AGB stars can have forsterite abundances of 12% by mass and higher, which is more than the previously found maximum abundance of 5%." @default.
• W3103946412 created "2020-11-23" @default.
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• W3103946412 date "2010-06-01" @default.
• W3103946412 modified "2023-10-03" @default.
• W3103946412 title "Determining the forsterite abundance of the dust around asymptotic giant branch stars" @default.
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• W3103946412 doi "https://doi.org/10.1051/0004-6361/200913588" @default.
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