6 papers
Effects on vsini determinations of O stars from 3D model atmospheres with high turbulent velocities
L. Delbroek, J. O. Sundqvist, F. Backs +3
When studying massive stars and their life cycles, rotation plays a key role. Hence, understanding the rotation of these stars is crucial when determining their properties, or for…
Simulations of massive star atmospheres and winds during giant eruptive and quiescent luminous blue variable phases
P. Schillemans, J. O. Sundqvist, D. Debnath +3
Mass loss from massive stars located in the part of the Hertzsprung-Russell diagram (HRD) where we find luminous blue variables (LBVs) is profoundly important for stellar evolution…
Spectral synthesis of 3D unified model atmospheres with winds for O stars
L. Delbroek, J. O. Sundqvist, D. Debnath +5
Spectroscopic studies of massive and luminous O-type stellar atmospheres and winds have primarily been done by using 1D, spherically symmetric and stationary models. Both observati…
An on-the-fly line-driven-wind iterative mass-loss estimator (LIME) for hot, massive stars of arbitrary chemical compositions
J. O. Sundqvist, D. Debnath, F. Backs +7
Mass-loss rates from hot, massive stars are important for a range of astrophysical applications. We present \href{https://lime.ster.kuleuven.be/}{LIME}, a fast, efficient, and easy…
Improving 1D stellar atmosphere models with insights from multi-dimensional simulations II. 1D versus 3D hydrodynamically consistent model comparison for WR stars
G. González-TorÃ, A. A. C. Sander, N. Moens +8
Classical Wolf-Rayet (cWR) stars are evolved massive stars that have lost most of their H envelope and exhibit dense, extended atmospheres with strong, line-driven winds. Accuratel…
Improving 1D stellar atmosphere models with insights from multi-dimensional simulations I. 1D vs 2D stratifications and spectral comparison for O stars
G. González-TorÃ, A. A. C. Sander, J. O. Sundqvist +7
We compare current 1D and multi-dimensional atmosphere modelling approaches for massive stars to understand their strengths and shortcomings. We calculate averaged stratifications…