Evolution and Nucleosynthesis of Very Massive Stars

TL;DR

This paper reviews the evolution and nucleosynthesis of very massive stars (over 100 solar masses), emphasizing the effects of metallicity, mass loss, and rotation on their life cycle and end states, including Wolf-Rayet stars and potential pair-instability supernovae.

Contribution

It provides a comprehensive analysis of VMS evolution, highlighting the roles of mass loss and metallicity, and discusses their nucleosynthesis and final outcomes based on recent models.

Findings

VMS have large convective cores and evolve homogeneously without rotational mixing.

At solar metallicity, VMS lose most of their mass and end as Wolf-Rayet stars.

Lower metallicity allows VMS to retain more mass, possibly leading to pair-instability supernovae.

Abstract

In this chapter, after a brief introduction and overview of stellar evolution, we discuss the evolution and nucleosynthesis of very massive stars (VMS: M>100 solar masses) in the context of recent stellar evolution model calculations. This chapter covers the following aspects: general properties, evolution of surface properties, late central evolution, and nucleosynthesis including their dependence on metallicity, mass loss and rotation. Since very massive stars have very large convective cores during the main-sequence phase, their evolution is not so much affected by rotational mixing, but more by mass loss through stellar winds. Their evolution is never far from a homogeneous evolution even without rotational mixing. All VMS at metallicities close to solar end their life as WC(-WO) type Wolf-Rayet stars. Due to very important mass loss through stellar winds, these stars may have luminosities during the advanced phases of their evolution similar to stars with initial masses between 60 and 120 solar masses. A distinctive feature which may be used to disentangle Wolf-Rayet stars originating from VMS from those originating from lower initial masses is the enhanced abundances of neon and magnesium at the surface of WC stars. At solar metallicity, mass loss is so strong that even if a star is born with several hundred solar masses, it will end its life with less than 50 solar masses (using current mass loss prescriptions). At the metallicity of the LMC and lower, on the other hand, mass loss is weaker and might enable star to undergo pair-instability supernovae.