Dust coagulation in star formation with different metallicities

Abstract

Dust grains coagulate into larger aggregates in dense gas. This changes their size distribution and possibly affects the thermal evolution of star-forming clouds. We here investigate dust coagulation in collapsing pre-stellar cores with different metallicities by considering the thermal motions of grains. We show that coagulation does occur even at low metallicity $\sim 10^{-6} \Zsun$. However, we also find (i) that the H${}_2$ formation rate on dust grains is reduced only after the majority of H${}_2$ is formed; and (ii) that the dust opacity is modified only after the core becomes optically thick. Therefore, we conclude that the effects of dust coagulation can safely be neglected in discussing the temperature evolution of the pre-stellar cores for any metallicity as long as the grain motions are thermal.

7 pages, 3 figures. Accepted for publication in MNRAS

References in corpus (4)

• Fragmentation of star-forming clouds enriched with the first dust
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• Dust coagulation in protoplanetary disks: porosity matters
• Shattering and coagulation of dust grains in interstellar turbulence

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