Dark Matter Densities during the Formation of the First Stars and in Dark Stars
Katherine Freese, Paolo Gondolo, J. A. Sellwood, Douglas Spolyar

TL;DR
This paper models dark matter density profiles during the formation of the first stars, showing that dark matter annihilation could power a 'Dark Star' phase, influencing early stellar evolution.
Contribution
It applies an adiabatic infall algorithm considering non-circular motions to estimate dark matter densities during first star formation, supporting the dark matter annihilation heating hypothesis.
Findings
Dark matter densities are sufficient for annihilation heating in first stars.
Dark matter profiles are within a factor of two of classical adiabatic contraction models.
Dark matter annihilation could prevent the collapse of the first stars to fusion stages.
Abstract
The first stars in the universe form inside dark matter (DM) haloes whose initial density profiles are laid down by gravitational collapse in hierarchical structure formation scenarios. During the formation of the first stars in the universe, the baryonic infall compresses the dark matter further. The resultant dark matter density is presented here, using an algorithm originally developed by Young to calculate changes to the profile as the result of adiabatic infall in a spherical halo model; the Young prescription takes into account the non-circular motions of halo particles. The density profiles obtained in this way are found to be within a factor of two of those obtained using the simple adiabatic contraction prescription of Blumenthal et al. Our results hold regardless of the nature of the dark matter or its interactions and rely merely on gravity. If the dark…
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