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- W4309134741 abstract "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." @default.
- W4309134741 created "2022-11-23" @default.
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- W4309134741 date "2022-11-14" @default.
- W4309134741 modified "2023-10-14" @default.
- W4309134741 title "Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities" @default.
- W4309134741 doi "https://doi.org/10.48550/arxiv.2211.07305" @default.
- W4309134741 hasPublicationYear "2022" @default.
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