Mineralogy of an OH/IR superwind

11th Pacific Rim Conference on Stellar Astrophysics: Physics and Chemistry of the Late Stages of Stellar Evolution

物理学;天文学

Lombaert, R.^1 ; De Vries, B.L.^2 ; Hillen, M.^3

Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, Onsala

439 92, Sweden^1

ESA, Scientific Support Office, Direct. of Science and Robotic Exploration, European Space Research and Technology Centre (ESTEC/SRE-S), Keplerlaan 1, AZ Noordwijk

2201, Netherlands^2

KU Leuven, Instituut voor Sterrenkunde, Celestijnenlaan 200D B-2401, Leuven

3001, Belgium^3

关键词: Continuum emission;    Dust formation;    OH/IR stars;    Preliminary model;    Spectral energy distribution;    Stellar wind;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/728/2/022004/pdf
DOI  :  10.1088/1742-6596/728/2/022004

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

The mineralogy of the dense, dusty superwind of OH/IR stars can provide important constraints for understanding the dust formation process as well as the acceleration of the wind. We aim to model the ISO-SWS spectrum of the OH/IR star OH 30.1-0.7 in detail by reproducing the slope of the spectral energy distribution in the continuum regions between 3 and 8 μm and 12 and 15 μm. In addition to metallic Fe, we find that larger amorphous olivine grains of size on the order of 1 μm may also contribute to the continuum emission. We report here on the preliminary model results and discuss their validity given the important assumption of a 1D spherically symmetric stellar wind.