论文标题
由于分散的偏心蛋白磁盘引起的行星偏心的共振激发：产生大行星偏心率的新机制
Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
论文作者
论文摘要
我们提出了产生大行星偏心率的新机制。该机制适用于其伴随原球磁盘内部空腔内的行星。由于与气体冷却相关的非绝热效应，具有内部截断的大磁盘可能会变得偏心，并且可以将其偏心保留在长期相干的偏心模式下。随着磁盘的分散，当行星和磁盘具有相同的Apsidal进动率时，内行星将与偏心磁盘遇到世俗的共鸣；然后，随着系统通过共振，行星的偏心率会兴奋至巨大的价值。在这项工作中，我们为广泛的质量求解了模型磁盘的偏心模式。然后，我们采用近似的世俗动力学模型来计算“行星 +分散磁盘”系统的长期演变。尽管磁盘偏心率很小（$ \ lyssim0.05 $），但在我们的计算中，地球在计算中达到了较大的偏心率（0.1至0.6之间）。可以通过模式转换（``避免过境''）现象与“行星 +磁盘”怪异特征性相关的现象来理解这种偏心性激发。
We present a new mechanism of generating large planetary eccentricities. This mechanism applies to planets within the inner cavities of their companion protoplanetary disks. A massive disk with an inner truncation may become eccentric due to non-adiabatic effects associated with gas cooling, and can retain its eccentricity in long-lived coherently-precessing eccentric modes; as the disk disperses, the inner planet will encounter a secular resonance with the eccentric disk when the planet and the disk have the same apsidal precession rates; the eccentricity of the planet is then excited to a large value as the system goes through the resonance. In this work, we solve the eccentric modes of a model disk for a wide range of masses. We then adopt an approximate secular dynamics model to calculate the long-term evolution of the "planet + dispersing disk" system. The planet attains a large eccentricity (between 0.1 and 0.6) in our calculations, even though the disk eccentricity is quite small ($\lesssim0.05$). This eccentricity excitation can be understood in terms of the mode conversion (``avoided crossing'') phenomenon associated with the evolution of the "planet + disk" eccentricity eigenstates.
