The maximum black hole mass at solar metallicity

Abstract

We analyse the current knowledge and uncertainties in detailed stellar evolution and wind modelling to evaluate the mass of the most massive stellar black hole (BH) at solar metallicity. Contrary to common expectations that it is the most massive stars that produce the most massive BHs, we find that the maximum M BH Max ≃ 30 ± 10 M ⊙ is found in the canonical intermediate range between M ZAMS ≃ 30 and 50 M ⊙ instead. The prime reason for this seemingly counter-intuitive finding is that very massive stars (VMS) have increasingly high mass-loss rates that lead to substantial mass evaporation before they expire as stars and end as lighter BHs than their canonical O-star counterparts.

Topics & Concepts