A Study of Primordial Very Massive Star Evolution

Abstract

We present new evolutionary models of primordial very massive stars with initial masses ranging from 100 to 1000 M _⊙ that extend from the main sequence to 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 ≈40 to ≈1000 M _⊙ . In particular, stars with initial masses of about 100 M _⊙ could leave black holes of ≃85–90 M _⊙ , values consistent with the estimated primary black hole mass of the GW190521 merger event. Overall, these results may contribute to explaining future data from next-generation gravitational-wave detectors, such as the Einstein Telescope and Cosmic Explorer, which will have access to an as-yet-unexplored black hole mass range of ≈10 ^2 –10 ^4 M _⊙ in the early universe.

Keywords

• Stellar evolution
• Stellar remnants
• Stellar winds
• Population III stars