Modeling DACs in UV Lines of Massive Hot Stars

Details Modeling DACs in UV Lines of Massive Hot Stars Modeling DACs in UV Lines of Massive Hot Stars

2007-07-25

arxiv.org/abs/0707.3779v1

Astronomy and Astrophysics

Astrophysics

3 pages, 3 figures. To appear in Clumping in Hot Star Winds, Proc. of Int. Workshop, 18-22 June 2007, Potsdam, Universitats-Ve

Scientific paper

We apply the 3-dimensional radiative transport code Wind3D to 3D hydrodynamic models of Corotating Interaction Regions to fit the detailed variability of Discrete Absorption Components observed in Si IV UV resonance lines of HD 64760 (B0.5 Ib). We discuss important effects of the hydrodynamic input parameters on these large-scale equatorial wind structures that determine the detailed morphology of the DACs computed with 3D transfer. The best fit model reveals that the CIR in HD 64760 is produced by a source at the base of the wind that lags behind the stellar surface rotation. The non-corotating coherent wind structure is an extended density wave produced by a local increase of only 0.6 % in the smooth symmetric wind mass-loss rate.

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