Convective differential rotation in stars and planets - I. Theory
Convective differential rotation in stars and planets - I. Theory
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恒星和行星中的对流差动旋转 - I. 理论
DOI：
10.1093/mnras/staa2323
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发表时间：
2020
影响因子：
4.8
通讯作者：
Jermyn A
中科院分区：
文献类型：
--
作者：
Jermyn A
我们推导出的尺度的微分旋转在缓慢和快速旋转对流区使用数量级的方法。我们的计算适用于恒星和流体行星和所有旋转速率，以及磁化和纯流体动力系统。我们发现剪力|R Ω|慢转系统的角频率为Ω| N|，其中N是Brünt-Väisälä频率，并发现对于快速旋转系统，它以Ω的幂律下降，Ω为|N|.进一步计算了纬向环流率和斜压性，并考察了快速旋转极限下的磁场强度。我们的结果与模拟和观测结果基本一致，我们与同伴论文中的结果进行了详细的比较。
We derive the scaling of differential rotation in both slowly and rapidly rotating convection zones using order of magnitude methods. Our calculations apply across stars and fluid planets and all rotation rates, as well as to both magnetized and purely hydrodynamic systems. We find shear |R∇Ω| of order the angular frequency Ω for slowly rotating systems with Ω ≪ |N|, whereNis the Brünt–Väisälä frequency, and find that it declines as a power law in Ω for rapidly rotating systems with Ω ≫ |N|. We further calculate the meridional circulation rate and baroclinicity and examine the magnetic field strength in the rapidly rotating limit. Our results are in general agreement with simulations and observations and we perform a detailed comparison with those in a companion paper.