The flow structure in the asynchronous polar CD Ind was investigated in the approximation of an offset dipole. Computation results made it possible to identify such system features as the drift of hot spots over the white dwarf surface, the flow structure dependence on the phase of the beat period, and the magnetic pole switching. To study the flow structure, a three-dimensional numerical MHD model based on the approximation of modified magnetic hydrodynamics was used. Numerical calculations were performed for ten phases of the beat period at a constant rate of mass transfer. In addition, for a more detailed study of the poles switching, additional calculation series were carried out in the corresponding phase ranges of the beat period. The energy release zones during the spin-orbit period shift in longitude on average by 20°, which corresponds to 0.05 of the orbital period phase. The magnetic pole switching occurs in a time that does not exceed 0.1 of the beat period. In the middle of this process, accretion occurs on both poles with the same intensity, and the flow resembles an arch. Based on the calculation results, synthetic light curves were constructed for the optical range of the spectrum.

异步极化CD Ind中的流动结构是在偏移偶极子近似下进行研究的。计算结果使得可以识别这样的系统特征，例如白矮星表面上的热点漂移，流动结构取决于拍频周期的相位以及磁极切换。为了研究流动结构，使用了基于修正磁流体动力学近似的三维数值MHD模型。以恒定的传质速率对拍频周期的十个阶段进行了数值计算。此外，为了更详细地研究极点切换，在拍频周期的相应相位范围内进行了其他计算系列。自旋轨道期间的能量释放区平均在经度上移动20°，对应于轨道周期相位的0.05。磁极切换发生的时间不超过拍频周期的0.1。在此过程的中间，在两个极点上都以相同的强度发生增生，并且流动类似于弓形。根据计算结果，针对光谱的光学范围构建了合成光曲线。