Star formation and molecular hydrogen in dwarf galaxies: a non-equilibrium view

Abstract

We study the connection of star formation to atomic (HI) and molecular hydrogen (H${}_2$) in isolated, low metallicity dwarf galaxies with high-resolution ($m_{\mathrm{gas}}$ = 4 M${}_{\odot }$, $N_{\mathrm{ngb}}$ = 100) SPH simulations. The model includes self-gravity, non-equilibrium cooling, shielding from an interstellar radiation field, the chemistry of H${}_2$ formation, H${}_2$-independent star formation, supernova feedback and metal enrichment. We find that the H${}_2$ mass fraction is sensitive to the adopted dust-to-gas ratio and the strength of the interstellar radiation field, while the star formation rate is not. Star formation is regulated by stellar feedback, keeping the gas out of thermal equilibrium for densities $n<$ 1 cm${}^{-3}$. Because of the long chemical timescales, the H${}_2$ mass remains out of chemical equilibrium throughout the simulation. Star formation is well-correlated with cold ( T $⩽$ 100 K ) gas, but this dense and cold gas - the reservoir for star formation - is dominated by HI, not H${}_2$. In addition, a significant fraction of H${}_2$ resides in a diffuse, warm phase, which is not star-forming. The ISM is dominated by warm gas (100 K $<$ T $⩽3\times 10^4$ K) both in mass and in volume. The scale height of the gaseous disc increases with radius while the cold gas is always confined to a thin layer in the mid-plane. The cold gas fraction is regulated by feedback at small radii and by the assumed radiation field at large radii. The decreasing cold gas fractions result in a rapid increase in depletion time (up to 100 Gyrs) for total gas surface densities ${\Sigma }_{\mathrm{HI}+{\mathrm{H}}_2}\lesssim$ 10 M${}_{\odot }$pc${}^{-2}$, in agreement with observations of dwarf galaxies in the Kennicutt-Schmidt plane.

arXiv commentAccepted for publication in MNRAS. Changes (including a pamameter study in Appendix C) highlighted

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