Formation and Structure of Circumplanetary Disks and Envelopes during the Late Stages of Giant Planet Formation
arXiv:2403.05662 · doi:10.1016/j.icarus.2024.116044
Abstract
Giant planets are expected to form within circumstellar disks, which shape their formation history and the local environment. Here, we consider the formation and structure of circumplanetary disks that arise during the late stages of giant planet formation. During this phase, when most of the final mass is accumulated, incoming material enters the Hill sphere and falls toward the planet. In the absence of torques, the falling parcels of gas conserve their specific angular momentum and collect into a circumplanetary disk. Generalizing previous work, we consider a range of possible geometries for the flow entering the sphere of influence of the planet. Specifically, we consider five geometric patterns for the inward flow, ranging from concentration toward the rotational poles of the system to isotropic flow to concentration along the equatorial plane. For each case, we derive analytic descriptions for the density field of the infall region, the disk surface density in the absence of viscosity, and steady-state solutions for viscous disks. These results, in turn, specify the luminosity contributions of the planet, the circumplanetary disk, and the envelope. These power sources, in conjunction with the surrounding material, collectively determine the observational appearance of the forming planet. We conclude with an approximate determination of these radiative signatures.
arXiv comment19 pages, 9 figures. Published at Icarus
References in corpus (26)
- Rosseland and Planck Mean Opacities for Protoplanetary Discs
- On the Luminosity of Young Jupiters
- Disk Accretion Onto High-Mass Planets
- Three-dimensional Calculations of High and Low-mass Planets Embedded in Protoplanetary Discs
- A Circumplanetary Disk Around PDS70c
- Distribution of Accreting Gas and Angular Momentum onto Circumplanetary Disks
- How Empty are Disk Gaps Opened by Giant Planets?
- Nested-grid calculations of disk-planet interaction
- Accreting Circumplanetary Disks: Observational Signatures
- Circumplanetary disc properties obtained from radiation hydrodynamical simulations of gas accretion by protoplanets
- Reduced gas accretion on super-Earths and ice giants
- Circumplanetary disk or circumplanetary envelope?
- Tidal Truncation of Circumplanetary Discs
- Hydrodynamics of embedded planets' first atmospheres - III. The role of radiation transport for super-Earth planets
- Do Proto-Jovian Planets Drive Outflows?
- Angular Momentum Accretion onto a Gas Giant Planet
- On the Radio Detectability of Circumplanetary Discs
- Formation of Giant Planet Satellites
- Estimating the magnetic field strength in hot Jupiters
- Circumplanetary Disk Dynamics in the Isothermal and Adiabatic Limits
- Quasi-static contraction during runaway gas accretion onto giant planets
- Observability of Forming Planets and their Circumplanetary Disks II. -- SEDs and Near-Infrared Fluxes
- Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
- Accreting protoplanets: Spectral signatures and magnitude of gas and dust extinction at H alpha
- The Planetary Accretion Shock. III. Smoothing-free 2.5D simulations and calculation of H alpha emission
- The 3D dust and opacity distribution of protoplanets in multi-fluid global simulations