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arXiv · 1711.11287

Winds of Massive Magnetic Stars: Interacting Fields and Flow

Simon Daley-Yates·Ian Stevens
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Abstract

We present results of 3D numerical simulations of magnetically confined, radiatively driven stellar winds of massive stars, conducted using the astrophysical MHD code Pluto, with a focus on understanding the rotational variability of radio and sub-mm emission. Radiative driving is implemented according to the Castor, Abbott and Klein theory of radiatively driven winds. Many magnetic massive stars posses a magnetic axis which is inclined with respect to the rotational axis. This misalignment leads to a complex wind structure as magnetic confinement, centrifugal acceleration and radiative driving act to channel the circumstellar plasma into a warped disk whose observable properties should be apparent in multiple wavelengths. This structure is analysed to calculate free-free thermal radio emission and determine the characteristic intensity maps and radio light curves.

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Simon Daley-Yates, Ian Stevens. 2017-11-30. Winds of Massive Magnetic Stars: Interacting Fields and Flow. https://arxiv.org/abs/1711.11287

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