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High-resolution spectra of the magnetic star HD191612 were acquired using theChandra X-ray observatory at both maximum and minimum emission phases. Weconfirm the flux and hardness variations previously reported with XMM-Newton,demonstrating the great repeatability of the behavior of HD191612 over adecade. The line profiles appear typical for magnetic massive stars: nosignificant line shift, relatively narrow lines for high-Z elements, andformation radius at about 2R*. Line ratios confirm the softening of the X-rayspectrum at the minimum emission phase. Shift or width variations appear oflimited amplitude at most (slightly lower velocity and slightly increasedbroadening at minimum emission phase, but within 1--2 sigma of values atmaximum). In addition, a fully self-consistent 3D magnetohydrodynamic (MHD)simulation of the confined wind in HD191612 was performed. The simulationresults were directly fitted to the data leading to a remarkable agreementoverall between them.

Chandra View of Magnetically Confined Wind in HD191612: Theory versus Observations