Hot star wind mass-loss rate predictions at low metallicity
| Authors | |
|---|---|
| Year of publication | 2019 |
| Type | Article in Proceedings |
| Conference | Symposium S344 (Dwarf Galaxies: From the Deep Universe to the Present) |
| MU Faculty or unit | |
| Citation | |
| Web | https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/hot-star-wind-massloss-rate-predictions-at-low-metallicity/807E05435835B5ECDBE565C4DBA7EE4D |
| Doi | http://dx.doi.org/10.1017/S1743921318005331 |
| Keywords | Stars: winds; outflows; stars: mass-loss; stars: early-type; Magellanic Clouds; hydrodynamics; radiative transfer |
| Description | Hot star winds are driven by the radiative force due to light absorption in lines of heavier elements. Therefore, the amount of mass lost by the star per unit of time, i.e., the mass-loss rate, is sensitive to metallicity. We provide mass-loss rate predictions for O stars with mass fraction of heavier elements 0.2 |
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