Can very massive stars avoid Pair-Instability Supernovae?
arXiv:0801.3397 · doi:10.1017/S1743921308020516
Abstract
Very massive primordial stars (140 Msol < M < 260 Msol) are supposed to end their lives as PISN. Such an event can be traced by a typical chemical signature in low metallicity stars, but at the present time, this signature is lacking in the extremely metal-poor stars we are able to observe. Does it mean that those very massive objects were not formed, contrarily to the primordial star formation scenarios ? Could it be possible that they avoided this tragical fate ? We explore the effects of rotation, anisotropical mass loss and magnetic field on the core size of very massive Population III models. We find that magnetic fields provide the strong coupling that is lacking in standard evolution metal-free models and our 150 Msol Population III model avoids indeed the pair-instability explosion.
6 pages, 3 figures, proceedings of the IAU Symposium 250 "Massive stars as cosmic engines"
References in corpus (11)
- How Massive Single Stars End their Life
- The Nucleosynthetic Signature of Population III
- The Formation of the First Star in the Universe
- Low Temperature Opacities
- The Formation of the First Stars. I. The Primordial Star Forming Cloud
- Formation of Primordial Stars in a LCDM Universe
- On the Initial Mass Function of Population III Stars
- Line-driven winds, ionizing fluxes and UV-spectra of hot stars at extremely low metallicity. I. Very massive O-stars
- Population III star formation in a Lambda CDM universe, I: The effect of formation redshift and environment on protostellar accretion rate
- Implications of the metallicity dependence of Wolf-Rayet winds
- Nucleosynthesis, Reionization, and the Mass Function of the First Stars