Circumplanetary Disks Around Wide-Orbit Planets: Formation Theory, Observations, And Moon Systems

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Scientific paper

Using radiation hydrodynamics simulations, we explore the evolution of circumplanetary disks around wide-orbit substellar companions. At large distances from the star (r 100 AU), gravitational instability followed by disk fragmentation can form gas giants and/or brown dwarfs that are likely to host large, circumplanetary disks. These subdisks are not only affected by the tidal potential of the primary, but can also be gravitationally unstable, leading to nonaxisymmetric spiral structure. These spiral waves redistribute circumplanetary disk mass and can cause repeated heating events in the otherwise cold subdisk. We examine the evolutionary timescales for these circumplanetary disks, as well as the role that they play in regulating the growth of the substellar companions. In addition, we explore the effects that the resulting shock structures have on the thermal history of the gas, with application to ice grain physics, disk chemistry, and moon composition. Finally, the time scale for disk evolution affects the observability of these objects, increasing flux densities to be well within ALMA capabilities. The evolution of circumplanetary disks is fundamental to formation theories for massive planets and brown dwarfs. Moreover, large circumplanetary disks leave open the possibility for the formation of extensive moon systems, potentially including moons sufficiently massive to retain an atmosphere.

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