Standard spectroscopic methods for O-star vsini and macroturbulence only reliably measure the quantity sqrt(v_mac^2/2 + vsini^2/4) when neither clearly dominates, requiring re-analysis of prior rotation distributions.
Since we work with3 rot,in, the rotation at the inner bound- ary, we also refer to this method as the ‘inner boundary rotation’ method
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Effects on vsini determinations of O stars from 3D model atmospheres with high turbulent velocities
Standard spectroscopic methods for O-star vsini and macroturbulence only reliably measure the quantity sqrt(v_mac^2/2 + vsini^2/4) when neither clearly dominates, requiring re-analysis of prior rotation distributions.