Dark-matter halo mergers as a fertile environment for low-mass Population III star formation

Abstract

While Population III stars are typically thought to be massive, pathways towards lower-mass Pop III stars may exist when the cooling of the gas is particularly enhanced. A possible route is enhanced HD cooling during the merging of dark-matter halos. The mergers can lead to a high ionization degree catalysing the formation of HD molecules and may cool the gas down to the cosmic microwave background (CMB) temperature. In this paper, we investigate the merging of mini-halos with masses of a few 10${}^5$ M${}_{\odot }$ and explore the feasibility of this scenario. We have performed three-dimensional cosmological hydrodynamics calculations with the ENZO code, solving the thermal and chemical evolution of the gas by employing the astrochemistry package KROME. Our results show that the HD abundance is increased by two orders of magnitude compared to the no-merging case and the halo cools down to $\sim$60 K triggering fragmentation. Based on Jeans estimates the expected stellar masses are about 10 M${}_{\odot }$. Our findings show that the merging scenario is a potential pathway for the formation of low-mass stars.

Submitted to MNRAS

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• The formation of massive primordial stars in the presence of moderate UV backgrounds
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• Low-metallicity star formation: Relative impact of metals and magnetic fields
• Magnetic fields in primordial accretion disks
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• Massive black hole formation in Population III star clusters
• Do fragmentation and accretion affect the stellar Initial Mass Function?
• The chemical evolution of self-gravitating primordial disks