Vertical shear instability
The line integral convolution of the gas velocity shows the characteristic motions triggered by the vertical shear instability (Flores-Rivera et al. 2020).
VSI related works in our group
Flock et al. 2017
Flock et al. 2020
Flores, Flock et al. 2020
Barraza-Alfaro, Flock et al. 2021
Melon Fuksman, Flock & Klahr 2024a
Melon Fuksman, Flock & Klahr 2024b
Barraza-Alfaro, Flock et al. 2024
Gas dynamics in magnetized disks
The movie shows the turbulent evolution of a protoplanetary disk.
25 frames per second cover a simulation time of 1 year (1 inner orbit). Turbulent velocities are presented in units of the local Mach number. In the low-density upper layers of the disc, the turbulent flows are transonic with even supersonic peaks. In the bulk of the disk at the midplane, the turbulent velocities reach 10 % of the local Mach number. This set of simulations is calculated in the perfect coupling regime between gas and magnetic fields. They are scale-free! Turbulent magnetic fields are presented in the plasma beta evolution. For more information please refer to Flock et al. 2011.
Magnetic energy
The movies show the evolution of the magnetic energy in magnetized protoplanetary disks. Rendering was done using raytracing techniques with a scaling of the opacity proportional to the magnetic energy.
