Planets locked in the 3:2 orbital resonance that start moving outward from within 1-2 AU may reach beyond Almost-Equal-To 5 AU only under favorable conditions. For migrating planets locked in the 3:2 mean motion resonance, there are stalling radii that depend on disk viscosity and on stellar irradiation, when it determines the disk's thermal balance. Letters Additional Journal Information: Journal Volume: 918 Journal Issue: 2 Journal ID: ISSN 2041-8205 Publisher: IOP Publishing Country of Publication: United States Language: English Subject: 79 ASTRONOMY AND ASTROPHYSICS planet-disk interactions protoplanetary disks circumstellar disks planet = and/or by reducing the accretion rate toward the star, and hence depleting the inner disk. (LANL), Los Alamos, NM (United States) Sponsoring Org.: USDOE National Nuclear Security Administration (NNSA) USDOE Laboratory Directed Research and Development (LDRD) Program' National Science Foundation (NSF) National Aeronautics and Space Administration (NASA) OSTI Identifier: 1868223 Report Number(s): LA-UR-20-29630 Journal ID: ISSN 2041-8205 Grant/Contract Number: 89233218CNA000001 CHE-2039044 AST-1352369 NNX14AD21G PHY-1726951 Resource Type: Accepted Manuscript Journal Name: The Astrophysical Journal. Publication Date: Fri Sep 17 00:00: Research Org.: Los Alamos National Lab. Northwestern Univ., Evanston, IL (United States) Adolfo Ibáñez Univ., Santiago (Chile).Northwestern Univ., Evanston, IL (United States).Our results suggest that the many super-Jupiters observed by direct imaging at large distances from the star may have gotten there by outward migration. As a result, the torque on the inner disk dominates, and the planet pushes itself outward. In an eccentric disk, the torque on the outer disk weakens due to two effects: the planet launches weaker waves, and those waves travel further before damping. We show that, for planets on circular orbits, the transition from inward to outward migration coincides with the known transition from circular to eccentric disks that occurs for planets more massive than a few Jupiters. Our result differs from previous ones because of our longer simulation times, lower viscosity, and boundary conditions that allow the disk to reach a viscous steady state. Here we show that at higher masses, planets migrate outward. We report recent simulations show that giant planets of about 1 M J migrate inward at a rate that differs from the type II prediction.
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