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Baroclinically-driven flows and dynamo action in rotating spherical fluid shells

机译:旋转球形流体壳体中的斜压驱动流动和发电机动作

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摘要

The dynamics of stably stratified stellar radiative zones is of considerable interest due to the availability of increasingly detailed observations of Solar and stellar interiors. This article reports the first non-axisymmetric and time-dependent simulations of flows of anelastic fluids driven by baroclinic torques in stably stratified rotating spherical shells – a system serving as an elemental model of a stellar radiative zone. With increasing baroclinicity a sequence of bifurcations from simpler to more complex flows is found in which some of the available symmetries of the problem are broken subsequently. The poloidal component of the flow grows relative to the dominant toroidal component with increasing baroclinicity. The possibility of magnetic field generation thus arises and this paper proceeds to provide some indications for self-sustained dynamo action in baroclinically-driven flows. We speculate that magnetic fields in stably stratified stellar interiors are thus not necessarily of fossil origin as it is often assumed.
机译:稳定分层的恒星辐射区的动力学引起人们极大的兴趣,这是因为对太阳和恒星内部的观测越来越详细。本文报道了在稳定分层旋转球壳中由斜压驱动的非弹性流体流动的第一个非轴对称和随时间变化的模拟,该系统用作恒星辐射带的基本模型。随着斜压的增加,发现了从简单流向更复杂流的分叉序列,其中一些可用的对称问题随后被打破。流量的极向分量相对于主要环面分量随着斜压增加而增长。因此出现了产生磁场的可能性,并且本文继续为斜压驱动流中的自持发电机作用提供一些指示。我们推测,稳定分层的恒星内部的磁场因此不一定像通常所认为的那样是化石起源的。

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