Collaborative Study of Solar Turbulent Convection and Differential Rotation

研究人员对高湍流对流进行了详细的数值模拟，以解决类太阳恒星在差动自转中旋转和对流发挥的产额相互作用。这种具有非常高空间分辨率的模拟是由GAFD湍流团队在新的计算代码和程序上实现的，强调了在像太阳对流区这样复杂的动力系统中近似的物理的不同方面。科罗拉多团队使用了一种滞弹性球谐程序，旨在以高分辨率处理球壳中的复杂流动。明尼苏达团队使用完全可压缩的分段抛物线方法代码，将带有对流包络的整个旋转恒星放置在非常均匀的笛卡尔网格的中间。两者都允许包括磁场效应，以及前瞻性地研究发生在对流区深处的磁发电机过程，以及在恒星表面附近可见的影响。

Investigators make detailed numerical simulations of highly turbulent convection in resolving the yield interactions of rotation and convection play in differential rotation in solar-like stars. Such simulations with very high spatial resolution, enabled by the GAFD Turbulence team on new computational codes and procedures, emphasize on different aspects of the physics approximated in a dynamical system as complex as the solar convection zone. The Colorado team employs an anelastic spherical harmonic code, designed to deal with complex flows at high resolution in spherical shells. The Minnesota team uses a fully compressible Piecewise-Parabolic Method code, where an entire rotating star with a convective envelope is placed in the middle of a very fin uniform Cartesian grid. Both allow magnetic field effects to be included, as well, to prospectively study magnetic dynamo processes taking place deep in the convection zone, and effects visible near the stellar surface.