Clumpy Disc and Bulge Formation

Understand

We present a set of hydrodynamical/Nbody controlled simulations of isolated gas rich galaxies that self-consistently include SN feedback and a detailed chemical evolution model, both tested in cosmological simulations.

• The initial conditions are motivated by the observed star forming galaxies at z ~ 2-3.
• We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which in general, are not easily disrupted on timescales compared to the migration time.
• We show that stellar clumps migrate towards the central region and contribute to form a classical-like bulge with a Sersic index, n > 2.