Formation of HD molecules in merging dark matter haloes

Abstract

HD molecules can be an important cooling agent of the primordial gas behind the shock waves originated through mergings of the dark matter haloes at epochs when first luminous objects were to form. We study the necessary conditions for the HD cooling to switch on in the low temperature range $T<200$ K. We show that these conditions are fulfiled in merging haloes with the total (dark matter and baryon) mass in excess of $M_{\rm cr}\sim 10^7[(1+z)/20]^{-2}\msun$. Haloes with masses $M>M_{\mathrm{cr}}$ may be the sites of low-mass star formation.

arXiv comment9 pages, 7 figures, corrected version, accepted in MNRAS

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• Pre-galactic metal enrichment - The chemical signatures of the first stars
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• Metal and molecule cooling in simulations of structure formation
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• Is H3+ cooling ever important in primordial gas?
• Suppression of HD-cooling in protogalactic gas clouds by Lyman-Werner radiation
• The role of HD cooling in primordial star formation
• Planets in the Early Universe
• Chemistry of heavy elements in the Dark Ages
• Dark-matter halo mergers as a fertile environment for low-mass Population III star formation
• First supernovae in dwarf protogalaxies
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• State-to-state vibrational kinetics of H${}_2$ and H${}_2^{+}$ in a post-shock cooling gas with primordial composition
• Dark matter merging induced turbulence as an efficient engine for gas cooling
• Molecular fluorine chemistry in the early Universe
• Evolution of the First Supernovae in Protogalaxies: Dynamics of Mixing of Heavy Elements
• Astrophysics in 2006
• Mapping the Universe in HD
• Open questions in the study of population III star formation
• Over-cooled haloes at z > 10: a route to form low-mass first stars
• Self-Similar Shocks and Winds in Galaxy Clusters
• Instabilities in the Ionization Zones Around the First Stars
• Low-temperature primordial gas in merging halos
• The First Stars
• The role of gas fragmentation during the formation of supermassive black holes