Modelling magnetically channeled winds in 3D – I. Isothermal simulations of a magnetic O supergiant
Modelling magnetically channeled winds in 3D – I. Isothermal simulations of a magnetic O supergiant
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在 3D 中模拟磁引导风 — I. 磁 O 超巨星的等温模拟
DOI：
10.1093/mnras/stac1778
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发表时间：
2022
影响因子：
4.8
通讯作者：
Gagné, Marc
中科院分区：
文献类型：
--
作者：
Subramanian, Sethupathy;Balsara, Dinshaw S.;ud-Doula, Asif;Gagné, Marc
在本文中，我们提出了第一套三维磁流体动力学（MHD）模拟与黎曼geomeshcode进行。我们研究的磁通道风的磁性大质量恒星在全三维使用的代码，是唯一适合于球形问题的动力学。具体来说，我们进行等温模拟的平滑风旋转星星与倾斜，最初的偶极场。我们比较的质量损失，角动量损失，和磁层动力学的模板星星（与属性，让人想起的O4超巨星PUP）在一系列的旋转速率，磁场强度，和磁倾斜角。模拟运行到一个准稳态，观察到的结果与现有的文献是一致的，显示情节离心爆发事件的质量流出，由磁场回路，形成封闭的磁层的星星的限制。编目的结果提供的角度如何角动量损失的不同配置的旋转速率，磁场强度，和大的磁倾斜角的变化。与以前的二维MHD研究一致，我们发现，高磁约束降低了整体质量损失率，更高的旋转增加了质量损失率。这项研究和未来的研究将被用来估计角动量演化，自旋时间，和质量损失的演变的磁性大质量恒星的磁场强度，旋转速率和偶极倾斜的函数。
In this paper we present the first set of 3D magnetohydrodynamic (MHD) simulations performed with theriemann geomeshcode. We study the dynamics of the magnetically channeled winds of magnetic massive stars in full three dimensions using a code that is uniquely suited to spherical problems. Specifically, we perform isothermal simulations of a smooth wind on a rotating star with a tilted, initially dipolar field. We compare the mass-loss, angular momentum loss, and magnetospheric dynamics of a template star (with the properties that are reminiscent of the O4 supergiant ζ Pup) over a range of rotation rates, magnetic field strengths, and magnetic tilt angles. The simulations are run up to a quasi-steady state and the results are observed to be consistent with the existing literature, showing the episodic centrifugal breakout events of the mass outflow, confined by the magnetic field loops that form the closed magnetosphere of the star. The catalogued results provide perspective on how angular-momentum loss varies for different configurations of rotation rate, magnetic field strength, and large magnetic tilt angles. In agreement with previous 2D MHD studies, we find that high magnetic confinement reduces the overall mass-loss rate, and higher rotation increases the mass-loss rate. This and future studies will be used to estimate the angular-momentum evolution, spin-down time, and mass-loss evolution of magnetic massive stars as a function of magnetic field strength, rotation rate, and dipole tilt.