Three-dimensional modeling of radiative disks in binaries

TL;DR

This paper presents 3D simulations of circumstellar disks in binary systems, revealing how companion-induced perturbations affect disk morphology, temperature, and potential planet formation processes.

Contribution

It introduces an improved SPH code with radiative transfer to study binary disk evolution, highlighting the impact of binary separation on disk dynamics and thermal properties.

Findings

Spiral shock waves develop near pericenter.

Hydraulic jumps significantly heat the disks.

Binary separation influences disk morphology and temperature.

Abstract

Circumstellar disks in binaries are perturbed by the companion gravity causing significant alterations of the disk morphology. Spiral waves due to the companion tidal force also develop in the vertical direction and affect the disk temperature profile. These effects may significantly influence the process of planet formation. We perform 3D numerical simulations of disks in binaries with different initial dynamical configurations and physical parameters. Our goal is to investigate their evolution and their propensity to grow planets. We use an improved version of the SPH code VINE modified to better account for momentum and energy conservation. The energy equation includes a flux--limited radiative transfer algorithm and the disk cooling is obtained via "boundary particles". We model a system made of star/disk + star/disk where the secondary star (and relative disk) is less massive than the primary. The numerical simulations performed for different values of binary separation and disk density show that the disk morphology is substantially affected by the companion perturbations. Trailing spiral shock waves develop when the stars approach their pericenter. Strong hydraulic jumps occur at the shock front creating breaking waves and a consistent mass stream between the two disks, significantly heating them. The high gas temperature may prevent the ice condensation by moving outward the "snow line". The hydraulic jumps may slow down or even halt the dust coagulation process. At apocenter these perturbations are reduced and the disks are cooled down and less eccentric. The strength of the hydraulic jumps, disk heating, and mass exchange depends on the binary separation, and for larger semi-major axes, the tidal spiral pattern is substantially reduced.