Modeling Stellar Wind Spectra from Rapidly Rotating Stars
2024
Wolf-Rainer Hamann | Ludwig Schulz | Helge Todt
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.
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