Monday

It has been speculated that in extreme low-metallicity cloud environments, stars form in regions that are cold and dense, but dominated by atomic hydrogen instead of molecular. In this talk I will present a suite of 3D, high-resolution, (M)HD AREPO simulations of an isolated dwarf galaxy with time dependent chemistry. We vary the metallicity, UV, and whether magnetic fields are included to investigate the effect on star formation. In contrast to previous work, varying the UV field and metallicity does alter the star formation rate in our simulated dwarf galaxies. Moreover- changing these quantities leads to a Kennicutt-Schmidt relationship with a shallower slope. To investigate in detail the origin of these variations, we then present a detailed study of the local gas environment of our sink particles (representing small ~1pc gravitationally bound star forming clumps of gas) with regard to their mass, temperature, chemical composition, and local turbulence. To finish I will present an analysis of how the global star formation in such a system might change with the inclusion of magnetic fields- and show that this leads to a substantial reduction of the burstiness of star formation.