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| Paper: |
Wind Models for Very Massive Stars in the Local Universe |
| Volume: |
465, Four Decades of Massive Star Research - A Scientific Meeting in Honor of Anthony J. Moffat |
| Page: |
207 |
| Authors: |
Vink, J. S.; Bestenlehner, J. M.; Gräfener, G.; de Koter, A.; Langer, N. |
| Abstract: |
Some studies have claimed the existence of a stellar upper-mass limit of 150 M☉.
A factor that is often overlooked concerns the issue that there might be a significant
difference between the present-day and the initial mass of the most massive stars — as
a result of mass loss.
The upper-mass limit may be substantially higher, possibly exceeding 200 M☉.
The issue of the upper mass-limit will however remain uncertain as long as there is only
limited quantitative knowledge of mass loss in close proximity to the
Eddington limit (Γ).
For this reason, we present mass-loss predictions from Monte Carlo radiative
transfer models for very massive stars up to 300 M☉.
Using our new dynamical approach, we find an upturn or “kink” in
the mass loss versus Γ dependence, at the point where our model
winds become optically thick.
These are the first mass-loss predictions where the transition from
optically thin O-star winds to optically thick Wolf-Rayet winds
has been resolved. |
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