Dust Grain Growth & Dusty Supernovae in Low-Metallicity Molecular Clouds

Abstract

We present 3-D hydrodynamical models of the evolution of superbubbles powered by stellar winds and supernovae from young coeval massive star clusters within low metallicity ($Z=0.02$Z${}_{\odot }$), clumpy molecular clouds. We explore the initial stages of the superbubble evolution, including the occurrence of pair-instability and core-collapse supernovae. Our aim is to study the occurrence of dust grain growth within orbiting dusty clumps, and in the superbubble's swept-up supershell. We also aim to address the survival of dust grains produced by sequential supernovae. The model accounts for the star cluster gravitational potential and self-gravity of the parent cloud. It also considers radiative cooling (including that induced by dust) and a state-of-the-art population synthesis model for the coeval cluster. As shown before, a superbubble embedded into a clumpy medium becomes highly distorted, expanding mostly due to the hot gas streaming through low density channels. Our results indicate that in the case of massive ($\sim 10^7$M${}_{\odot }$) molecular clouds, hosting a super star cluster ($\sim 5.6\times 10^5$M${}_{\odot }$), grain growth increments the dust mass at a rate $\sim 4.8\times 10^{-5}$M${}_{\odot }$ yr${}^{-1}$ during the first $2.5$Myr of the superbubble's evolution, while the net contribution of pair-instability and core-collapse supernovae to the superbubble's dust budget is $\sim 1200$M${}_{\odot }(M_{SC}/5.6\times 10^5$M${}_{\odot })$, where $M_{SC}$ is the stellar mass of the starburst. Therefore, dust grain growth and dust injection by supernovae lead to create, without invoking a top-heavy initial mass function, massive amounts of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust mass present in galaxies soon after the onset of cosmic reionization.

arXiv comment8 pages, 4 figures. Accepted for publication in The Astrophysical Journal

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