Rotation Profiles of Solar-like Stars with Magnetic Fields
Rotation Profiles of Solar-like Stars with Magnetic Fields
复制标题
具有磁场的类太阳恒星的自转剖面
DOI：
10.1088/1009-9271/8/6/06
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发表时间：
2008
期刊：
影响因子：
--
通讯作者：
Shaolan Bi
中科院分区：
文献类型：
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作者：
Wuming Yang;Shaolan Bi
研究了类太阳恒星在磁场作用下的自转轮廓。导出了磁角动量输运的扩散系数。计算了不同质量的旋转恒星模型的自转剖面。只考虑流体动力学不稳定性的太阳模型的总角动量约为太阳年龄时的13倍，且不能再现辐射区的准固体转动。然而，具有磁场的太阳模型不仅可以再现辐射区域中几乎均匀的旋转，而且还可以再现与太阳年龄3 σ水平的日震结果一致的总角动量。类太阳恒星在磁场作用下的自转在辐射区几乎是均匀的，但对于1.2-1.5 M（圆点）的模型，在对流核和辐射区之间有一个明显的过渡区，在那里角速度有一个急剧的径向梯度，这与太阳和大质量恒星在磁场作用下的自转轮廓不同。过渡区角速度的变化随年龄和质量的增加而增大。
We investigate the rotation profile of solar-like stars with magnetic fields. A diffusion coefficient of magnetic angular momentum transport is deduced. Rotating stellar models with different mass incorporating the coefficient are computed to give the rotation profiles. The total angular momentum of a solar model with only hydrodynamic instabilities is about 13 times larger than that of the Sun at the age of the Sun, and this model can not reproduce quasi-solid rotation in the radiative region. However, the solar model with magnetic fields not only can reproduce an almost uniform rotation in the radiative region, but also a total angular momentum that is consistent with the helioseismic result at the 3 sigma level at the age of the Sun. The rotation of solar-like stars with magnetic fields is almost uniform in the radiative region, but for models of 1.2-1.5 M(circle dot), there is an obvious transition region between the convective core and the radiative region, where angular velocity has a sharp radial gradient, which is different from the rotation profile of the Sun and of massive stars with magnetic fields. The change of angular velocity in the transition region increases with increasing age and mass.