Simulations of the line-driven instability in magnetic hot star winds

Context. Line-driven winds of hot, luminous stars are intrinsically unstable due to the line-deshadowing instability (LDI). In non-magnetic hot stars, LDI leads formation an inhomogeneous wind consisting small-scale, spatially separated clumps that can have great effects on observational diagnostics. However, for magnetic generated structures, dynamics, and diagnostics not been directly investigated so far. Aims. We non-linear development structures dynamics in a line-driven typical O-supergiant. Methods. employed two-dimensional axisymmetric magnetohydrodynamic simulations using Smooth Source Function approximation evaluating assumed one-dimensional line force. To facilitate interpretation these models, they were compared with corresponding simulation as well neglecting LDI. Results. A central result obtained is morphology clumping properties change strongly increasing wind-magnetic confinement. Most notably, magnetically confined flows, large-scale, shellular sheets (‘pancakes’) quite distinct from separate, small-scale winds. discuss impact findings diagnostic studies stellar evolution models stars.