期刊
ASTRONOMY & ASTROPHYSICS
卷 516, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/200913588
关键词
AGB and post-AGB; stars: mass-loss; astrochemistry; radiative transfer; infrared: stars
资金
- Fund for Scientific Research of Flanders (FWO) [G.0470.07]
- STFC [ST/F003196/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F003196/1] Funding Source: researchfish
Aims. 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. Methods. 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 mu m forsterite bands, that probe the most recent (11.3 mu m) and older (33.6 mu m) mass-loss history of the star. Simple diagnostic diagrams are derived, allowing direct comparison to observed band strengths. Results. Our analysis shows that the 11.3 mu 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 mu 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%.
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