A Study of Primordial Very Massive Star Evolution

Understand

We present new evolutionary models of primordial very massive stars, with initial masses ranging from $100\,\mathrm{{M}_{\odot}}$ to $1000\,\mathrm{{M}_{\odot}}$, that extend from the main sequence until the onset of dynamical instability caused by the creation of electron-positron pairs during core C, Ne, or O burning, depending on the star's mass and metallicity.

• Mass loss accounts for radiation-driven winds as well as pulsation-driven mass-loss on the main sequence and during the red supergiant phase.
• After examining the evolutionary properties, we focus on the final outcome of the models and associated compact remnants.
• Stars that avoid the pair-instability supernova channel, should produce black holes with masses ranging from $\approx 40\, \mathrm{{M}_{\odot}}$ to $\approx 1000\,\mathrm{{M}_{\odot}}$.