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Context. Towards the end of their evolution, hot massive stars develop strong stellar winds and appear as emission line stars, such as Wolf-Rayet (WR) stars or luminous blue variables (LBVs). The quantitative description of the mass loss in these important pre-supernova phases is hampered by unknowns, such as clumping and porosity due to an inhomogeneous wind structure and by an incomplete theoretical understanding of optically thick stellar winds. Even the stellar radii in these phases are badly understood since they are often variable (LBVs) or deviate from theoretical expectations (WR stars).
Gräfener et al. (Thu,) studied this question.
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