标题： 质量流量和吸积通过吸积盘中的间隙 显示英文标题

标题： Mass Flow and Accretion through gaps in Accretion Discs

摘要： 我们研究了原行星在吸积盘中形成的间隙的结构和动力学。 求解了一个具有嵌入的木星大小原行星的平坦、二维、非自引力原恒星吸积盘的流体动力学方程，该原行星位于圆形轨道上。 为了模拟质量可能向原行星的吸积，我们持续从行星的洛希瓣内部移除质量，并对其进行监控。 首先，展示了可以得到与数值问题（如边界条件或初始条件、人工粘性或分辨率）无关的一致结果。 然后，详细参数研究描述了盘粘度和压力对吸积率大小的影响。 我们发现，即使在盘中形成了间隙，行星仍然能够从盘中吸积更多质量。 这种吸积发生在行星轨道半径的径向外部和内部区域。 吸积率取决于粘度的大小和盘的垂直厚度。 对于盘粘度 alpha=10^{-3}和垂直厚度 H/r=0.05，我们估计积累一个木星质量的时间尺度约为十万年。 对于更大的（更小的）粘度和盘厚度，这种吸积率会增加（减少）。 对于非常小的粘度（alpha < 5 10^{-4}），通过间隙向行星的吸积率显著降低，相应的吸积时间尺度变得比盘的粘性演化时间更长。 显示英文摘要

摘要： We study the structure and dynamics of the gap created by a protoplanet in an accretion disc. The hydrodynamic equations for a flat, two-dimensional, non-selfgravitating protostellar accretion disc with an embedded, Jupiter sized protoplanet on a circular orbit are solved. To simulate possible accretion of mass onto the protoplanet we continually remove mass from the interior of the planet's Roche lobe which is monitored. Firstly, it is shown that consistent results independent on numerical issues (such as boundary or initial conditions, artificial viscosity or resolution) can be obtained. Then, a detailed parameter study delineates the influence of the disc viscosity and pressure on the magnitude of the accretion rate. We find that, even after the formation of a gap in the disc, the planet is still able to accrete more mass from the disc. This accretion occurs from regions of the disc which are radially exterior and interior to the planet's orbital radius. The rate depends on the magnitude of the viscosity and vertical thickness of the disc. For a disc viscosity alpha=10^{-3} and vertical thickness H/r=0.05 we estimate the time scale for the accumulation of one Jupiter mass to be of order hundred thousand years. For a larger(smaller) viscosity and disc thickness this accretion rate is increasing(decreasing). For a very small viscosity (alpha < 5 10^{-4}) the mass accretion rate through the gap onto the planet is markedly reduced, and the corresponding accretion time scale becomes larger than the viscous evolution time of the disc.