On the operation of the chemothermal instability in primordial star-forming clouds
Thomas H. Greif, Volker Springel, Volker Bromm

TL;DR
This study uses 3D simulations to explore how chemothermal instability influences fragmentation in primordial star-forming clouds, revealing conditions that lead to early gravitational collapse and clump formation.
Contribution
It provides new insights into the role of chemothermal instability in primordial clouds and highlights the potential for early fragmentation during initial collapse phases.
Findings
Chemothermal instability causes a dip in cooling time, promoting fragmentation.
Secondary clumps can form and potentially collapse independently.
Fragmentation likelihood varies among different primordial haloes.
Abstract
We investigate the operation of the chemothermal instability in primordial star-forming clouds with a suite of three-dimensional, moving-mesh simulations. In line with previous studies, we find that the gas at the centre of high-redshift minihaloes becomes chemothermally unstable as three-body reactions convert the atomic hydrogen into a fully molecular gas. The competition between the increasing rate at which the gas cools and the increasing optical depth to H2 line emission creates a characteristic dip in the cooling time over the free-fall time on a scale of 100 au. As a result, the free-fall time decreases to below the sound-crossing time, and the cloud may become gravitationally unstable and fragment on a scale of a few tens of au during the initial free-fall phase. In three of the nine haloes investigated, secondary clumps condense out of the parent cloud, which will likely…
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