Mass loss implementation and temperature evolution of very massive stars

Abstract

Massive stars with initial masses above 100 M _⊙ dominate the physics of young clusters by outputting enormous amounts of mechanical and chemical feedback into their surroundings. The mass lost by these very massive stars (VMS) in their winds determine their evolution, chemical yields and their end fates. In this contribution we study the main-sequence (MS) evolution of VMS with a new mass-loss recipe based on the model-independent transition mass loss observed in the Arches and 30 Dor cluster in the Galaxy and Large Magellanic Cloud (LMC) respectively.