论文标题
基于动力摩擦的行星盘相互作用，针对行星轨道迁移和偏心型的新的简单处方
A new and simple prescription for planet orbital migration and eccentricity damping by planet-disc interactions based on dynamical friction
论文作者
论文摘要
在行星形成期间，行星胚胎与原球星盘之间的重力相互作用引起行星胚胎的轨道迁移，该胚胎在塑造最终行星系统中起着重要作用。虽然迁移有时发生在超音速状态中，但行星胚胎和气体之间的相对速度高于声速，但迄今为止提出的迁移处方描述了行星盘相互作用的相互作用力和轨道上的轨道变化，超音速状态的轨道变化是不一致的。在这里，我们讨论了文献中现有处方的详细信息，并为基于动力摩擦的行星 - 盘相互作用提供了一种新的简单和直观的公式，可以在超音速和亚音速案例中应用。当现有处方采用特定的光盘模型时，我们的纸张包括对光盘参数的明确依赖性；因此，它可以应用于任何径向表面密度和温度依赖性的圆盘（除了径向尺度小于圆盘尺度高的局部变化外）。我们的处方将减少来自行星迁移的不同文献制剂的不确定性，并将成为研究行星吸收过程的重要工具，尤其是在研究近距离系统中通常发现的近距离低质量行星的形成时。
During planet formation gravitational interaction between a planetary embryo and the protoplanetary gas disc causes orbital migration of the planetary embryo, which plays an important role in shaping the final planetary system. While migration sometimes occurs in the supersonic regime, wherein the relative velocity between the planetary embryo and the gas is higher than the sound speed, migration prescriptions proposed thus far describing the planet-disc interaction force and the timescales of orbital change in the supersonic regime are inconsistent with one another. Here we discuss the details of existing prescriptions in the literature and derive a new simple and intuitive formulation for planet-disc interactions based on dynamical friction that can be applied in both supersonic and subsonic cases. While the existing prescriptions assume particular disc models, ours include the explicit dependence on the disc parameters; hence it can be applied to discs with any radial surface density and temperature dependence (except for the local variations with radial scales less than the disc scale height). Our prescription will reduce the uncertainty originating from different literature formulations of planet migration and will be an important tool to study planet accretion processes, especially when studying the formation of close-in low-mass planets that are commonly found in exoplanetary systems.
