木星生长模型消除热力学和流体动力学约束
Models of Jupiter's Growth Incorporating Thermal and Hydrodynamic Constraints
摘要：
[摘要]我们通过核心成核吸积来模拟木星的增长，应用来自磁盘-行星相互作用的流体动力学过程的约束。我们使用Henyey类型的恒星演化代码计算行星的内部结构。行星与原行星盘的相互作用使用3-D流体动力学模拟计算。以前的木星增长模型都认为木星的半径大约是一个希尔球的半径。然而，三维流体动力学模拟显示，只有0.25Rhill范围内的气体仍然与行星结合，更远的气体最终参与了原行星盘的剪切流。因此，在我们的新模拟中，行星的外边界被放置在气体具有热能的位置，以到达不受行星约束的流动部分。我们发现，较小的半径将行星生长所需的时间增加约5%。热压力限制了一颗质量不到地球几十倍的行星从原行星盘中积累气体的速度，而流体动力学则控制着更大质量行星的生长速度。在一个中等粘性的圆盘中，当行星的质量大约等于土星的质量时，吸积率达到峰值。在一个粘性较小的圆盘中，吸积的流体动力学极限较小，吸积率在较低质量时达到峰值。考虑到磁盘耗散，我们执行我们的一些模拟木星的增长在磁盘的表面气体密度减少的时间尺度为300万年。根据我们的模拟，原木星的膨胀和热支持的信封太小，无法捕捉行星目前的不规则卫星的随从，如波拉克等人（1979）所主张的。
英文摘要：
[Abridged] We model the growth of Jupiter via core nucleated accretion, applying constraints from hydrodynamical processes that result from the disk-planet interaction. We compute the planet's internal structure using a Henyey-type stellar evolution code. The planet's interactions with the protoplanetary disk are calculated using 3-D hydrodynamic simulations. Previous models of Jupiter's growth have taken the radius of the planet to be approximately one Hill sphere radius, Rhill. However, 3-D hydrodynamic simulations show that only gas within 0.25Rhill remains bound to the planet, with the more distant gas eventually participating in the shear flow of the protoplanetary disk. Therefore in our new simulations, the planet's outer boundary is placed at the location where gas has the thermal energy to reach the portion of the flow not bound to the planet. We find that the smaller radius increases the time required for planetary growth by ~5%. Thermal pressure limits the rate at which a planet less than a few dozen times as massive as Earth can accumulate gas from the protoplanetary disk, whereas hydrodynamics regulates the growth rate for more massive planets. Within a moderately viscous disk, the accretion rate peaks when the planet's mass is about equal to the mass of Saturn. In a less viscous disk hydrodynamical limits to accretion are smaller, and the accretion rate peaks at lower mass. To account for disk dissipation, we perform some of our simulations of Jupiter's growth within a disk whose surface gas density decreases on a timescale of 3Myr. According to our simulations, proto-Jupiter's distended and thermally-supported envelope was too small to capture the planet's current retinue of irregular satellites as advocated by Pollack et al. (1979).
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