II。轴对称和空间变化平衡和流动对MHD波型的影响：圆柱几何
II. The effect of axisymmetric and spatially varying equilibria and flow on MHD wave modes: Cylindrical geometry
摘要：
磁流体动力学（MHD）波是太阳大气中经常观测到的现象。这些波在太阳物理学的背景下是重要的，因为人们普遍认为它们可以对太阳大气的能量预算做出贡献，并且是对日冕加热做出贡献的主要候选者。这些波的现实模型需要代表观察到的配置，使等离子体的性质可以更准确地确定，不能直接测量。这项工作利用以前开发的数值技术，找到不同的非均匀平衡条件下的笛卡尔磁板几何形状的可压缩本征值。在这里，我们调查的性质磁声波的非均匀平衡下的圆柱几何形状。以前获得的分析结果检索强调这种数值技术的力量和适用性。进一步的案例研究调查的效果，径向非均匀的等离子体密度和非均匀的等离子体流，建模为一系列的高斯分布，对不同的MHD波的属性。对于所有情况下的色散图和空间本征函数计算显示的平衡不均匀性的影响。结果表明，随着平衡非均匀性的增加，径向空间本征函数的影响和额外的节点介绍，类似于以前的调查的磁性板。此外，方位角扰动随着波导内引入涡旋运动的不均匀性的增加而增加。最后，2D和3D表示的速度场示出，这可能是有用的观察员波模式识别下的现实磁波导与不断增加的仪器分辨率。
英文摘要：
Magnetohydrodynamic (MHD) waves are routinely observed in the solar atmosphere. These waves are important in the context of solar physics as it is widely believed they can contribute to the energy budget of the solar atmosphere and are a prime candidate to contribute towards coronal heating. Realistic models of these waves are required representing observed configurations such that plasma properties can be determined more accurately which can not be measured directly. This work utilises a previously developed numerical technique to find permittable eigenvalues under different non-uniform equilibrium conditions in a Cartesian magnetic slab geometry. Here we investigate the properties of magnetoacoustic waves under non-uniform equilibria in a cylindrical geometry. Previously obtained analytical results are retrieved to emphasise the power and applicability of this numerical technique. Further case studies investigate the effect that a radially non-uniform plasma density and non-uniform plasma flow, modelled as a series of Gaussian profiles, has on the properties of different MHD waves. For all cases the dispersion diagrams are obtained and spatial eigenfunctions calculated which display the effects of the equilibrium inhomogeneity. It is shown that as the equilibrium non-uniformity is increased, the radial spatial eigenfunctions are affected and extra nodes introduced, similar to the previous investigation of a magnetic slab. Furthermore, azimuthal perturbations are increased with increasing inhomogeneity introducing vortical motions inside the waveguide. Finally, 2D and 3D representations of the velocity fields are shown which may be useful for observers for wave mode identification under realistic magnetic waveguides with ever increasing instrument resolution.
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