Mineralogy of an OH/IR superwind
Paper i proceeding, 2016

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.


Robin Lombaert

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

B. L. de Vries

European Space Research and Technology Centre (ESA ESTEC)

M. Hillen

KU Leuven

Journal of Physics: Conference Series

17426588 (ISSN) 17426596 (eISSN)

Vol. 728 2 022004


Astronomi, astrofysik och kosmologi



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