3-D Radiative Transfer Modelling of Massive-Star UV Wind Line Variability

We present detailed semi-empiric models for rotational modulations observed in ultraviolet wind lines of B0.5 supergiant HD64760. We model the Rotational Modulation Regions (RMRs) with advanced 3-D radiative transfer calculations in the stellar wind and quantitatively fit the time-evolution of the Si iv λ1395 resonance line. We find that the RMRs are due to linearly-shaped narrow sector-like density enhancements in the equatorial wind. Unlike the Co-rotating Interaction Regions (CIRs) which produce Discrete Absorption Components in the line, the RMRs do not spread out with larger distance above the stellar surface. The detailed best fit shows that the RMRs of HD64760 have maximum density enhancements of ∼17% above the surrounding smooth wind density, about twice smaller than the hydrodynamic models of CIRs that warp around the star. The semi-empiric 3-D transfer modelling reveals that the narrow spoke-like RMRs must co-exist with broader and curved large-scale CIR wind density structures in the equatorial plane of this fast rotating Ib-supergiant. Session: Atmospheres, mass loss and stellar winds Individual Objects: HD 64760, ξ Per, HD150168