![]() (LANL), Los Alamos, NM (United States) Sponsoring Org.: USDOE National Nuclear Security Administration (NNSA) USDOE Laboratory Directed Research and Development (LDRD) Program OSTI Identifier: 1711400 Report Number(s): LA-UR-20-24009 Journal ID: ISSN 1538-4357 TRN: US2204656 Grant/Contract Number: 89233218CNA000001 Resource Type: Journal Article: Accepted Manuscript Journal Name: The Astrophysical Journal (Online) Additional Journal Information: Journal Volume: 900 Journal Issue: 1 Journal ID: ISSN 1538-4357 Publisher: Institute of Physics (IOP) Country of Publication: United States Language: English Subject: 79 ASTRONOMY AND ASTROPHYSICS protoplanetary disks planet-disk interactions planet = star and is initially marginally unstable. Publication Date: Research Org.: Los Alamos National Lab. ![]() The player controls one of three anthropomorphic animal protagonists: the dragon girl Lilac, the wildcat Carol, or the basset hound Milla. of California, Santa Cruz, CA (United States) Tsinghua Univ., Beijing (China) Freedom Planet is a 2014 platform game developed and published by American video game designer Sabrina DiDuro, for her studio GalaxyTrail. of California, Santa Cruz, CA (United States) Origin Space Co. ![]() 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. Consequently, the intrinsic surface density distribution of the disk delicately determines both the pace and direction of the planets' type II migration. To make it clear, since we still get threads about this: The DLC is on indefinate hold. 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 more » near the gap walls preserve their magnitude. The associated gap profile modifies the location of corotation and Lindblad resonances. 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. 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. Moreover, numerical simulations indicate that the planets' migrations are not solely determined by the viscous diffusion of their natal 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. It is usually assumed that their type II migration is coupled to the viscous evolution of the disk. Proto–gas giant planets, with Hill radii larger than the disk thickness, open gaps and quench gas flow in the vicinity of their orbits. During their formation, emerging protoplanets tidally interact with their natal disks.
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