Chemical Enrichment of the Early IGM by Low-Mass Primordial Stars

Astronomy and Astrophysics – Astronomy

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Scientific paper

For now, primordial stars lie beyond the realm of direct observation, but indirect measures of their masses may be possible by analyzing their nucleosynthetic imprint on subsequent generations of low-mass long-lived stars, some of which may persist as extremely metal-poor (EMP) and hyper metal-poor (HMP) stars in the Galactic halo today. The absence of the "odd-even" abundance pattern of pair-instability SNe in metal-poor halo stars surveyed to date suggests that the early IGM was primarily enriched by low-mass stars. We present numerical simulations of spherically-symmetric core collapse SNe of 15 - 40 solar mass stars, surveying two progenitor rotation rates, three masses, two metallicities and three explosion energies, for a total of 36 models. We compare our nucleosynthetic yields to the chemical abundances of the three most iron-poor stars and match the abundance pattern of one, HE 0557-4840, with a zero-metallicity 15 solar mass, 2.4 Bethe explosion. A Salpeter IMF average of our yields for Z = 0 models with explosion energies of 2.4 Bethe or less is a good match to the abundances in the much larger sample of EMP stars. Since EMP stars likely carry the cumulative nucleosynthetic imprint of a few well-established populations of SNe progenitors, our findings suggest that low-mass SNe contributed the bulk of the metals to the early universe.

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