Document Type

Article

Publication Date

11-5-2020

Publication Title

Monthly Notices of the Royal Astronomical Society

Volume

500

Issue

3

First page number:

2822

Last page number:

2830

Abstract

© 2021 Oxford University Press. All rights reserved. We investigate whether the regular Galilean satellites could have formed in the dead zone of a circumplanetary disc. A dead zone is a region of weak turbulence in which the magnetorotational instability is suppressed, potentially an ideal environment for satellite formation. With the grid-based hydrodynamic code FARGO3D, we examine the evolution of a circumplanetary disc model with a dead zone. Material accumulates in the dead zone of the disc leading to a higher total mass and but a similar temperature profile compared to a fully turbulent disc model. The tidal torque increases the rate of mass transport through the dead zone leading to a steady-state disc with a dead zone that does not undergo accretion outbursts. We explore a range of disc, dead zone, and mass inflow parameters and find that the maximum mass of the disc is around 0.001MJ. Since the total solid mass of such a disc is much lower, we find that there is not sufficient material in the disc for in situ formation of the Galilean satellites and that external supplement is required.

Keywords

Accretion, accretion discs; Hydrodynamics; Methods: numerical; Planets and satellites: Composition; Planets and satellites: Formation

Disciplines

Stars, Interstellar Medium and the Galaxy

File Format

pdf

File Size

1654 KB

Language

English

Creative Commons License

Creative Commons Attribution 4.0 License
This work is licensed under a Creative Commons Attribution 4.0 License.

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