Stellar Signatures of Inhomogeneous Big Bang Nucleosynthesis. (arXiv:2006.02446v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Arbey_A/0/1/0/all/0/1">Alexandre Arbey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auffinger_J/0/1/0/all/0/1">Jérémy Auffinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silk_J/0/1/0/all/0/1">Joseph Silk</a>
We evaluate abundance anomalies generated in patches of the universe where
the baryon-to-photon ratio was locally enhanced by possibly many orders of
magnitude in the range $eta = 10^{-10} – 10^{-1}$. Our study is motivated by
the possible survival of rare dense regions in the early universe, the most
extreme of which, above a critical threshold, collapsed to form primordial
black holes. If this occurred, one may expect there to also be a significant
population of early-forming stars that formed in similar but subthreshold
patches. We derive a range of element abundance signatures by performing BBN
simulations at high values of the baryon-to-photon ratio that may be detectable
in any surviving first generation stars of around a solar mass. Our predictions
apply to metal-poor galactic halo stars, to old globular star clusters and to
dwarf galaxies, and we compare with observations in each of these cases.
We evaluate abundance anomalies generated in patches of the universe where
the baryon-to-photon ratio was locally enhanced by possibly many orders of
magnitude in the range $eta = 10^{-10} – 10^{-1}$. Our study is motivated by
the possible survival of rare dense regions in the early universe, the most
extreme of which, above a critical threshold, collapsed to form primordial
black holes. If this occurred, one may expect there to also be a significant
population of early-forming stars that formed in similar but subthreshold
patches. We derive a range of element abundance signatures by performing BBN
simulations at high values of the baryon-to-photon ratio that may be detectable
in any surviving first generation stars of around a solar mass. Our predictions
apply to metal-poor galactic halo stars, to old globular star clusters and to
dwarf galaxies, and we compare with observations in each of these cases.
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