Fig. 11.
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Spectroscopy of ε Ori showing the Hα line profile that is highly variable and can be in several morphologies, like P Cygni profile, inverse P Cygni profile, double emission, or pure emission (Thompson & Morrison 2013). It implies an intense wind (e.g. Puebla et al. 2016) or a decretion disk fed by mass loss from the star. This variable line was not used in our modelling.
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