We compare features from the circulation model developed in Stȩpień for contact binaries to a long-term hydrodynamical evolution of a symmetric contact binary. The numerical evolution is fully three-dimensional and begins from an equilibrium structure in contact at one grid cell. As the evolution is conducted with Flow-ER, an explicit hydrodynamics code for self-gravitating fluids, we are not able to address energy transport or evolution on a thermal timescale. However, we are able to investigate the width and height of the equatorial accretion belt and the flow of material in and out of the inner Lagrange point. The flow of material between the two components arises quickly in the evolution and does not change significantly through tens of orbital periods. As the stellar components are modeled as polytropes of index 3/2 a slight numerical mass imbalance causes one component to only gain mass over the course of the simulation leading eventually to a dynamical merger of the contact binary.

我们将 Stȩpień 开发的接触双星环流模型的特征与对称接触双星的长期流体动力学演化进行了比较。数值演化是完全三维的，从一个网格单元接触的平衡结构开始。由于演化是使用自引力流体的明确流体动力学代码 Flow-ER 进行的，因此我们无法解决热时间尺度上的能量传输或演化问题。然而，我们能够研究赤道吸积带的宽度和高度以及进出内拉格朗日点的物质流动。两种成分之间的物质流动在演化过程中迅速出现，并且在数十个轨道周期中不会发生显着变化。