Incorporating the molecular gas phase in galaxy-size numerical simulations: first applications in dwarf galaxies

Details Incorporating the molecular gas phase in galaxy-size numerical simulations: first applications in dwarf galaxies Incorporating the molecular gas phase in galaxy-size numerical simulations: first applications in dwarf galaxies

2006-03-21

arxiv.org/abs/astro-ph/0603581v1

Astrophys.J. 645 (2006) 1024-1042

Astronomy and Astrophysics

Astrophysics

46 pages, 14 figures (AASTEX); accepted for ApJ

Scientific paper

10.1086/504366

We present models of the evolution of the gaseous and stellar content of galaxies incorporating the formation of H_2 out of HI gas as part of such a model. We do so by formulating a subgrid model for gas clouds that uses well-known cloud scaling relations and solves for the HI-H_2 balance set by the H_2 formation on dust grains and its FUV-induced photodissociation by the temporally and spatially varying interstellar radiation field. This allows the seamless tracking of the evolution of the H_2 gas phase, its precursor Cold Neutral Medium (CNM) HI gas, simultaneously with the star formation. Our most important findings are: a) a significant dependence of the HI-H_2 transition and the resultant H_2 gas mass on the ambient metallicity and the H_2 formation rate, b) the important influence of the characteristic star formation timescale (regulating the ambient FUV radiation field) on the equilibrium H_2 gas mass and c) the possibility of a diffuse H_2 gas phase. Finally, we implement and briefly explore a novel approach of using the ambient H_2 gas mass fraction as a criterion for the onset of star formation. (abridged)

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