Shaping the structure of a GMC with radiation and winds

Abstract

We study the effect of stellar feedback (photodissociation/ionization, radiation pressure and winds) on the evolution of a Giant Molecular Cloud (GMC), by means of a 3D radiative transfer, hydro-simulation implementing a complex chemical network featuring ${\mathrm{H}}_2$ formation and destruction. We track the formation of individual stars with mass $M>1{\mathrm{M}}_{\odot }$ with a stochastic recipe. Each star emits radiation according to its spectrum, sampled with 10 photon bins from near-infrared to extreme ultra-violet bands; winds are implemented by energy injection in the neighbouring cells. We run a simulation of a GMC with mass $M=10^5{\mathrm{M}}_{\odot }$, following the evolution of different gas phases. Thanks to the simultaneous inclusion of different stellar feedback mechanisms, we identify two stages in the cloud evolution: (1) radiation and winds carve ionized, low-density bubbles around massive stars, while FUV radiation dissociates most ${\mathrm{H}}_2$ in the cloud, apart from dense, self-shielded clumps; (2) rapid star formation (SFR$\simeq 0.1{\mathrm{M}}_{\odot }{\mathrm{yr}}^{-1}$) consumes molecular gas in the dense clumps, so that UV radiation escapes and ionizes the remaining HI gas in the GMC. ${\mathrm{H}}_2$ is exhausted in $1.6$ Myr, yielding a final star formation efficiency of 36 per cent. The average intensity of FUV and ionizing fields increases almost steadily with time; by the end of the simulation ($t=2.5$ Myr) we find $⟨G_0⟩\simeq 10^3$ (in Habing units), and a ionization parameter $⟨U_{\mathrm{ion}}⟩\simeq 10^2$, respectively. The ionization field has also a more patchy distribution than the FUV one within the GMC. Throughout the evolution, the escape fraction of ionizing photons from the cloud is $f_{\mathrm{ion},\mathrm{esc}}<0.03$.

arXiv comment16 pages, 12 figures

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