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Abstract: The first stars in the universe form inside $\sim 10^6 M \odot$ dark matterDM haloes whose initial density profiles are laid down by gravitationalcollapse in hierarchical structure formation scenarios. During the formation ofthe first stars in the universe, the baryonic infall compresses the dark matterfurther. The resultant dark matter density is presented here, using analgorithm originally developed by Young to calculate changes to the profile asthe result of adiabatic infall in a spherical halo model; the Youngprescription takes into account the non-circular motions of halo particles. Thedensity profiles obtained in this way are found to be within a factor of two ofthose obtained using the simple adiabatic contraction prescription ofBlumenthal et al. Our results hold regardless of the nature of the dark matteror its interactions and rely merely on gravity. If the dark matter consists ofweakly interacting massive particles, which are their own antiparticles, theirdensities are high enough that their annihilation in the first protostars canindeed provide an important heat source and prevent the collapse all the way tofusion. In short, a ``Dark Star- phase of stellar evolution, powered by DMannihilation, may indeed describe the first stars in the universe.



Autor: Katherine Freese, Paolo Gondolo, J. A. Sellwood, Douglas Spolyar

Fuente: https://arxiv.org/



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