Reference : Chandra View of Magnetically Confined Wind in HD191612: Theory Versus Observations
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
Chandra View of Magnetically Confined Wind in HD191612: Theory Versus Observations
Nazé, Yaël mailto [Université de Liège > > Groupe d'astrophysique des hautes énergies (GAPHE) >]
ud-Doula, Asif [Penn State Worthington Scranton, Dunmore, PA 18512, USA <ID system="ORCID">0000-0001-7721-6713</ID>]
Zhekov, Svetozar A. [Institute of Astronomy and National Astronomical Observatory, 72 Tsarigradsko Chaussee Blvd., Sofia 1784, Bulgaria)]
Astrophysical Journal
IOP Publishing
Yes (verified by ORBi)
United Kingdom
[en] stars: early-type ; stars: individual: HD191612 ; stars: winds ; outflows ; X-rays: stars
[en] High-resolution spectra of the magnetic star HD 191612 were acquired using the Chandra X-ray Observatory at both maximum and minimum emission phases. We confirm the flux and hardness variations previously reported with XMM-Newton, demonstrating the high repeatability of the behavior of HD 191612 over a decade. The line profiles appear typical for magnetic massive stars: no significant line shift, relatively narrow lines for high-Z elements, and formation radius at about 2 {R}[SUB]* [/SUB]. Line ratios confirm the softening of the X-ray spectrum at the minimum emission phase. Shift or width variations appear of limited amplitude at most (slightly lower velocity and slightly increased broadening at minimum emission phase, but within 1–2σ of values at maximum). In addition, a fully self-consistent 3D magnetohydrodynamic simulation of the confined wind in HD 191612 was performed. The simulation results were directly fitted to the data, leading to a remarkable agreement overall between them.
Researchers ; Professionals

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