Retention of Long-period Gas Giant Planets: Type II Migration Revisited

Chen, Yi-Xian; Zhang, Xiaojia; Li, Yaping; Li, Hui; Lin, Douglas N. C.

doi:10.3847/1538-4357/abaab6

Retention of Long-period Gas Giant Planets: Type II Migration Revisited

Journal Article · Mon Aug 31 00:00:00 EDT 2020 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/abaab6· OSTI ID:1711400

^[1]; ^[2]; ^[3]; ^[3]; ^[4]

Tsinghua Univ., Beijing (China)
Univ. of California, Santa Cruz, CA (United States); Origin Space Co. Ltd. (China)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Univ. of California, Santa Cruz, CA (United States); Tsinghua Univ., Beijing (China)

During their formation, emerging protoplanets tidally interact with their natal disks. Proto–gas giant planets, with Hill radii larger than the disk thickness, open gaps and quench gas flow in the vicinity of their orbits. It is usually assumed that their type II migration is coupled to the viscous evolution of the disk. Although this hypothesis provides an explanation for the origin of close-in planets, it also encounters a predicament on the retention of long-period orbits for most gas giant planets. Moreover, numerical simulations indicate that the planets' migrations are not solely determined by the viscous diffusion of their natal disk. In this work, we carry out a series of hydrodynamic simulations combined with analytic studies to examine the transition between different paradigms of type II migration. We find a range of planetary mass for which gas continues to flow through a severely depleted gap so that the surface density distribution in the disk region beyond the gap is maintained in a quasi-steady state. The associated gap profile modifies the location of corotation and Lindblad resonances. In the proximity of the planet's orbit, high-order Lindblad and corotation torque are weakened by the gas depletion in the gap, while low-order Lindblad torques near the gap walls preserve their magnitude. Consequently, the intrinsic surface density distribution of the disk delicately determines both the pace and direction of the planets' type II migration. We show that this effect might stall the inward migration of giant planets and preserve them in disk regions where the surface density is steep.

View Accepted Manuscript (DOE)

Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE Laboratory Directed Research and Development (LDRD) Program; USDOE National Nuclear Security Administration (NNSA)

Grant/Contract Number:: 89233218CNA000001

OSTI ID:: 1711400

Report Number(s):: LA-UR--20-24009

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 1 Vol. 900; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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