![Cosmological Simulations Cosmological Simulations](/3547320/header_image-1433331081.jpg?t=eyJ3aWR0aCI6ODQ4LCJmaWxlX2V4dGVuc2lvbiI6ImpwZyIsIm9ial9pZCI6MzU0NzMyMH0%3D--5061d6dd8d4ecd9773552bcd7c88d6e7bc51c4fa)
Cosmological Simulations
![Projections of the stellar density for stars in a cosmological simulation grouped into nine different age bins. There is a trend from round (large scaleheight, short scalelength) to flattened (small scaleheight, long scalelength) distributions, when going from old to young sub-populations where stars are at z = 0 (co-eval populations).](/4485897/original-1518438322.jpg?t=eyJ3aWR0aCI6MjQ2LCJvYmpfaWQiOjQ0ODU4OTd9--0fb7da2efee4577bea5b81a00a1ce33d445a0656)
Projections of the stellar density for stars in a cosmological simulation grouped into nine different age bins. There is a trend from round (large scaleheight, short scalelength) to flattened (small scaleheight, long scalelength) distributions, when going from old to young sub-populations where stars are at z = 0 (co-eval populations).
MPIA/Stinson et al 2013
Cosmological simulations give a fuller understanding of consequential factors and processes in the formation and subsequent evolution of the Galaxy.