Effects of dust grain size distribution on the abundances of CO and H${}_2$ in galaxy evolution

Abstract

We model the effect of grain size distribution in a galaxy on the evolution of CO and H${}_2$ abundances. The formation and dissociation of CO and H${}_2$ in typical dense clouds are modelled in a manner consistent with the grain size distribution. The evolution of grain size distribution is calculated based on our previous model, which treats the galaxy as a one-zone object but includes various dust processing mechanisms in the interstellar medium (ISM). We find that typical dense clouds become fully molecular (H${}_2$) when the dust surface area increases by shattering while an increase of dust abundance by dust growth in the ISM is necessary for a significant rise of the CO abundance. Accordingly, the metallicity dependence of the CO-to-H${}_2$ conversion factor, $X_{\mathrm{CO}}$, is predominantly driven by dust growth. We also examine the effect of grain size distribution in the galaxy by changing the dense gas fraction, which controls the balance between coagulation and shattering, clarifying that the difference in the grain size distribution significantly affects $X_{\mathrm{CO}}$ even if the dust-to-gas ratio is the same. The star formation time-scale, which controls the speed of metal enrichment also affects the metallicity at which the CO abundance rapidly increases (or $X_{\mathrm{CO}}$ drops). We also propose dust-based formulae for $X_{\mathrm{CO}}$, which need further tests for establishing their usefulness.

arXiv comment14 pages, 7 figures, accepted for publication in MNRAS

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Cited by in corpus (1)

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