论文标题
在大规模磁场中嵌入的收缩恒星辐射区域中的角动量传输
Angular momentum transport in a contracting stellar radiative zone embedded in a large scale magnetic field
论文作者
论文摘要
人们认为，一些收缩或扩张的恒星在其辐射内部设有大规模的磁场。通过与收缩诱导的流相互作用，此类场可能会显着改变恒星的旋转历史。因此，它们构成了解决恒星进化快速阶段中角动量转运问题的一种有希望的方法。在这项工作中，我们旨在研究收缩辐射区域中的流和磁场之间的相互作用。我们提出了一个场景，该方案可能解释了类似太阳能恒星的后序列序列演化，其中在收缩时间范围内可以通过大规模磁场维持准固体旋转。然后，轴对称的不稳定性将破坏这种大规模的结构，并使差异旋转设置为差异。这种收缩驱动的不稳定性也可能是强烈和弱磁性中间质量恒星之间观察到的二分法的起源。
Some contracting or expanding stars are thought to host a large-scale magnetic field in their radiative interior. By interacting with the contraction-induced flows, such fields may significantly alter the rotational history of the star. They thus constitute a promising way to address the problem of angular momentum transport during the rapid phases of stellar evolution. In this work, we aim at studying the interplay between flows and magnetic fields in a contracting radiative zone. We propose a scenario that may account for the post-main sequence evolution of solar-like stars, in which a quasi-solid rotation can be maintained by a large-scale magnetic field during a contraction timescale. Then, an axisymmetric instability would destroy this large-scale structure and enables the differential rotation to set in. Such a contraction driven instability could also be at the origin of the observed dichotomy between strongly and weakly magnetic intermediate-mass stars.
