Open AccessAl 2 O 3 dust in OH/IR stars
Author(s) -
Maldoni M. M.,
Ireland T. R.,
Smith R. G.,
Robinson G.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09314.x
Subject(s) - physics , silicate , stars , astrophysics , asymptotic giant branch , circumstellar dust , radiative transfer , condensation , amorphous solid , population , kinetic energy , cosmic dust , astronomy , crystallography , chemistry , thermodynamics , demography , quantum mechanics , sociology
The presence of amorphous Al 2 O 3 in the shells of five OH/IR stars has been investigated via radiative transfer modelling of their respective spectral energy distributions (SEDs). The results show that the inclusion of this species in the models leads to excellent fits to the respective 10‐μm silicate bands as well as the region between the 10‐ and 20‐μm silicate bands. The formation of Al 2 O 3 , or Al–O bonds within early condensates, is an accepted feature of theoretical models of dust condensation in O‐rich dust shells, and while other metal oxides are not excluded, this study represents further evidence that this species may be present in the shells of high mass‐loss asymptotic giant branch (AGB) and post‐AGB stars. Significantly, it is found that the amorphous Al 2 O 3 grains are present as a distinct dust population. This may be the result of kinetic factors interrupting the dust condensation sequence at a stage which results in large amounts of Al 2 O 3 grains not being able to react with other species and thus being ejected in a pristine form.