在非等温盘中生长和运动的低质量行星
Growing and moving low-mass planets in non-isothermal disks
摘要：
我们通过辐射流体动力学模拟研究了低质量行星与原行星盘的相互作用，并对能量平衡进行了现实的处理。我们看看吸积和迁移率，并将其与等温研究进行比较。我们使用了三维版本的流体动力学方法RODEO，连同辐射传输的通量限制扩散的方法。吸积速率以及行星上的扭矩，关键取决于盘有效冷却的能力。对于太阳星云中适合于5 AU的密度，与等温模型相比，吸积率下降了一个数量级以上，而同时行星上的扭矩是正的，表明向外迁移。需要将密度降低2倍以恢复向内迁移，并且需要将密度降低2个数量级以上以恢复通常的I型迁移。力矩似乎与未扰动圆盘中的径向熵梯度成正比。这些发现对于原行星的生存至关重要，它们最终应该会进入人口合成模型。
英文摘要：
We study the interaction of a low-mass planet with a protoplanetary disk with a realistic treatment of the energy balance by doing radiation-hydrodynamical simulations. We look at accretion and migration rates and compare them to isothermal studies. We used a three-dimensional version of the hydrodynamical method RODEO, together with radiative transport in the flux-limited diffusion approach. The accretion rate, as well as the torque on the planet, depend critically on the ability of the disk to cool efficiently. For densities appropriate to 5 AU in the solar nebula, the accretion rate drops by more than an order of magnitude compared to isothermal models, while at the same time the torque on the planet is positive, indicating outward migration. It is necessary to lower the density by a factor of 2 to recover inward migration and more than 2 orders of magnitude to recover the usual Type I migration. The torque appears to be proportional to the radial entropy gradient in the unperturbed disk. These findings are critical for the survival of protoplanets, and they should ultimately find their way into population synthesis models.
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