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We present a new mechanism of generating large planetary eccentricities. Thismechanism applies to planets within the inner cavities of their companionprotoplanetary disks. A massive disk with an inner truncation may becomeeccentric due to non-adiabatic effects associated with gas cooling, and canretain its eccentricity in long-lived coherently-precessing eccentric modes; asthe disk disperses, the inner planet will encounter a secular resonance withthe eccentric disk when the planet and the disk have the same apsidalprecession rates; the eccentricity of the planet is then excited to a largevalue as the system goes through the resonance. In this work, we solve theeccentric modes of a model disk for a wide range of masses. We then adopt anapproximate 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 isquite small ($\lesssim0.05$). This eccentricity excitation can be understood interms of the mode conversion (``avoided crossing'') phenomenon associated withthe evolution of the "planet + disk" eccentricity eigenstates.

Resonant Excitation of Planetary Eccentricity due to a Dispersing  Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary  Eccentricities