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.

中文翻译：

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分散偏心原行星盘对行星偏心率的共振激发：一种新的大行星偏心率产生机制

我们提出了一种产生大行星偏心率的新机制。这种机制适用于其伴生原行星盘内腔内的行星。由于与气体冷却相关的非绝热效应，具有内部截断的大质量圆盘可能会变得偏心，并且可以在长寿命的相干进动偏心模式下保持其偏心；随着圆盘的分散，当行星和圆盘具有相同的拱点进动率时，内行星将与偏心圆盘发生长期共振；当系统经历共振时，行星的偏心率会被激发到一个很大的值。在这项工作中，我们解决了各种质量的模型盘的偏心模式。然后我们采用近似的长期动力学模型来计算“