Model of a Gap Formed by a Planet with Fast Inward Migration

Abstract

A planet is formed within a protoplanetary disk. Recent observations have revealed substructures such as gaps and rings, which may indicate forming planets within the disk. Due to disk-planet interaction, the planet migrates within the disk, which can affect a shape of the planet-induced gap. In this paper, we investigate effects of fast inward migration of the planet on the gap shape, by carrying out hydrodynamic simulations. We found that when the migration timescale is shorter than the timescale of the gap-opening, the orbital radius is shifted inward as compared to the radial location of the gap. We also found a scaling relation between the radial shift of the locations of the planet and the gap as a function of the ratio of the timescale of the migration and gapopening. Our scaling relation also enables us to constrain the gas surface density and the viscosity when the gap and the planet are observed. Moreover, we also found the scaling relation between the location of the secondary gap and the aspect ratio. By combining the radial shift and the secondary gap, we may constrain the physical condition of the planet formation and how the planet evolves in the protoplanetary disk, from the observational morphology.

High Spatial Resolution Observations of Molecular Lines toward the Protoplanetary Disk around TW Hya with ALMA

“…2c) is just beyond the region where the au-scale dust clump was discovered (52 au) in high spatial resolution dust continuum observations (Tsukagoshi et al 2019). Hydrodynamic simulations of planet-disk interaction suggests that the orbital radius of a planet with fast inward migration is shifted inward compared to the location of the gas gap if the migration time is shorter than the gapopening time (e.g., Kanagawa et al 2020). According to these hydrodynamic simulations, the difference between the locations of the planet and the gas gap depends on the planetto-stellar mass ratio, the local scale height of the gas disk, the local gas surface density, and the turbulent viscosity.…”

The evolution of large cavities and disc eccentricity in circumbinary discs

“…Conservation of angular momentum during infall on to the binary forces the material to form a disc. The binary exerts a tidal torque on the disc (Lin & Papaloizou 1979; Downloaded from https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/staa2954/5911605 by UQ Library user on 02 October 2020 Goldreich & Tremaine 1980), altering its structure by forming a gap (Crida et al 2006;Duffell 2015;Kanagawa et al 2020) or, if the binary mass ratio is sufficiently high, a cavity (Cuadra et al 2009;Shi et al 2012;D'Orazio et al 2013;Farris et al 2014;Miranda et al 2017). Vice versa, the disc exerts a back-reaction torque on the binary causing evolution of its orbital properties (migration, eccentricity evolution) and also producing characteristic accretion patterns (Artymowicz & Lubow 1996;Günther & Kley 2002;Farris et al 2014;Young et al 2015;Ragusa et al 2016;Muñoz et al 2019;Teyssandier & Lai 2019a).…”

PGNets: Planet mass prediction using convolutional neural networks for radio continuum observations of protoplanetary disks

“…Note that if we assume that one planet can carve two gaps (Dong et al 2018;Bae & Zhu 2018a,b) and the secondary gap is at 0.5 -0.7 r 𝑝 , we can input all the gaps into CNN models since our CNN models have been trained with data which have these secondary gaps generated by a single planet. The model does not consider migration, which can lead to a different gap shape (Nazari et al 2019;Kanagawa et al 2020). The gap substructure can also change with time.…”