Evolution and Nucleosynthesis of Very Massive Primordial Stars

Details Evolution and Nucleosynthesis of Very Massive Primordial Stars Evolution and Nucleosynthesis of Very Massive Primordial Stars

2000-10-10

arxiv.org/abs/astro-ph/0010206v1

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, LaTeX, requires espcrc1.sty. To appear in Nucl. Phys. A., the proceedings of the conference "Nuclei in the

Scientific paper

10.1016/S0375-9474(01)00697-2

We investigate the evolution, final fate, and nucleosynthetic yields of rotating and non-rotating very massive stars (VMS) of zero metallicity. First we address the issue of mass loss during hydrogen burning due to vibrational instabilities. We find that these objects are much more stable than what was found in previous studies of VMS of solar composition, and expect only negligible mass loss driven by the pulsations. As these stars thus reach the end of their evolution with massive helium cores, they encounter the pair-creation instability. We find that for helium core masses of ~64...133 solar masses these stars are completely disrupted with explosion energies of up to ~1E53 erg and eject up to ~60 solar masses of Ni56 Stars with more massive helium cores collapse into black holes. We present the first calculations that follow the collapse of such a massive rotating star and predict that X-ray burst and significant gravitational wave emission could result.

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