000002327 001__ 2327
000002327 005__ 20160701171703.0
000002327 037__ $$aASTROimport-484
000002327 100__ $$aBlomme, R.
000002327 245__ $$aNon-radial pulsations and large-scale structure in stellar winds
000002327 260__ $$c2009
000002327 520__ $$aAlmost all early-type stars show Discrete Absorption Components (DACs) in their ultraviolet spectral lines. These can be attributed to Co-rotating Interaction Regions (CIRs): large-scale spiral-shaped structures that sweep through the stellar wind. We used the Zeus hydrodynamical code to model the CIRs. In the model, the CIRs are caused by ``spots" on the stellar surface. Through the radiative acceleration these spots create fast streams in the stellar wind material. Where the fast and slow streams collide, a CIR is formed. By varying the parameters of the spots, we quantitatively fit the observed DACs in HD~64760. An important result from our work is that the spots do not rotate with the same velocity as the stellar surface. The fact that the cause of the CIRs is not fixed on the surface eliminates many potential explanations. The only remaining explanation is that the CIRs are due to the interference pattern of a number of non-radial pulsations. 
000002327 773__ $$c131$$pCommunications in Asteroseismology$$v158$$y2009
000002327 85642 $$ahttp://esoads.eso.org/abs/2009CoAst.158..131B
000002327 905__ $$apublished in
000002327 980__ $$aREFERD