Abstract
We present stellar evolution calculations for Population III stars for both single- and binary- star evolutions. Our models include 10- and 16.5-Msingle stars and a 10-Mmodel star that undergoes an episode of accretion resulting in a final mass of 16.1 M� . For comparison, we present the evolution of a solar heavy element abundance model. We use the structure from late-stage evolution models to calculate simulated supernova light curves. Light curve comparisons are made between accretion and non-accretion progenitor models, and models for single-star evolution of comparable masses. Where possible, we make comparisons to previous works. Similar investigations have been carried out, but primarily for solar or near-solar heavy metal abundance stars and not including both the evolution and the supernova explosions in one work.
Highlights
It is commonly believed that the first stars, Population III (Pop III) stars, were formed from primarily hydrogen and helium
We present the results of evolutionary calculations of 10- and 16.5-M stars with an initial total heavy element abundance Z = 10−15 from the pre-main sequence (pre-MS)
Similar to what we found for our single 16.5-M model, the first hydrogen pulse shown in Fig. 5 is accompanied by a growing convection zone, shown in Fig. 7, mixing down a fresh supply of protons
Summary
It is commonly believed that the first stars, Population III (Pop III) stars, were formed from primarily hydrogen and helium These zero heavy element abundance objects are of great interest for a variety of reasons. None the less, Omykai & Yoshii (2005) argue that many IMF determinations do not include feedback effects of massive stars already formed, which may induce lower mass fragmentation. For each evolved Pop III star, we use the structure from late-stage evolution as the starting point for simulation of their SN light curves.
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