Summary
In this case the disc galaxy is evolved in isolation and hence the morphology remains flocculent throughout the simulation time.Simulated using Arepo
Extreme Horizon
Resolving galactic disks in their cosmic environment
Orion
Molecular cloud fragmentation and evolution, formation of prestellar cores
Fragdisk
Fragmentation of self-gravitating disks
Synthetic disk populations
Resolving protoplanetary disks in massive protostellar clumps
Wind of HD189733
Unveiling the magnetic link between stars and planets
Dusty collapses
Understanding the dynamics of dust during the protostellar collapse