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- Modeling Stellar Wind Spectra from Rapidly Rotating Stars
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Modeling Stellar Wind Spectra from Rapidly Rotating Stars
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In post-interaction massive binaries (PIMBs) one often finds rapidly rotating objects, e.g., after one component has accreted mass and angular momentum, or after two components merged. Being hot and luminous, such objects drive stellar winds. Models for stellar atmospheres and winds usually adopt spherical symmetry. However, rapid rotation would break this symmetry.
We have developed a version of the Potsdam Wolf–Rayet (PoWR) model atmosphere code which allows to combine two different atmosphere models, e.g., one for the rapid wind over the polar regions, and a second one for the slower wind over the gravity-darkened equatorial zone.
For two examples we will demonstrate that such 1.5-D spectral simulations can explain observed wind-line profiles which otherwise cannot be reproduced.
This work is distributed under the Creative Commons CC BY 4.0 Licence.
Paper presented at the 41st Liège International Astrophysical Colloquium on “The eventful life of massive star multiples,” University of Liège (Belgium), 15–19 July 2024.
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Para citar este artículo
Acerca de: Wolf-Rainer Hamann
email : wrh@astro.physik.uni-potsdam.de