Can very massive stars avoid Pair-Instability Supernovae?

TL;DR

This study investigates whether very massive primordial stars can avoid pair-instability supernovae by examining the effects of rotation, anisotropic mass loss, and magnetic fields, finding magnetic fields enable some stars to escape this fate.

Contribution

The paper demonstrates that magnetic fields can significantly alter the evolution of very massive Population III stars, allowing them to avoid pair-instability supernovae, which was previously thought unavoidable.

Findings

Magnetic fields provide strong coupling in stellar cores.

150 Msol Population III model avoids pair-instability explosion.

Rotation and anisotropic mass loss effects are also considered.

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.