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Very massive stars (VMS) play a fundamental role in astrophysics due to theirwinds and supernovae (SN), and their role as massive black hole (BH)progenitors. However, their origin and evolution remain a significantchallenge. Recent theoretical work and observations suggest that VMSapproaching the Eddington limit may experience mass loss above the standardwind predictions. This study investigates how enhanced winds influence singleand binary VMS evolution, observable properties, and resulting BH populations.New stellar wind prescriptions, sensitive to the Eddington parameter($\Gamma_e$) and the luminosity-to-mass ratio, were implemented into thestellar evolution code PARSEC v2.0. These updated single-star tracks (100 - 600M$_{\odot}$ at Z=0.006) were used to model the VMS population in the TarantulaNebula and integrated into the SEVN binary evolution code. The$\Gamma_e$-enhanced single-star tracks match observed VMS properties betterthan standard models. Explaining the most massive star, R136a1, through asingle-star origin suggests a zero-age main sequence (ZAMS) mass limit of $<$400 M$_{\odot}$ regardless of the wind recipe used. However, binary stellarmergers also offer a suitable origin for R136a1 and other observed VMS,potentially lowering the upper ZAMS mass limit by ~100 M$_{\odot}$. Inbinaries, enhanced winds inhibit main-sequence stellar mergers and limit BHproduction above the pair-instability mass gap's lower edge (~50 M$_{\odot}$).Binary BHs merging in a Hubble time with enhanced winds yield more primary BHsabove 30 M$_{\odot}$ and enable secondary BHs between 30-40 solar masses, arange not found with standard stellar winds at LMC metallicity. This studyhighlights the crucial role that stellar winds and binary interactions play inVMS evolution and offers predictions relevant for interpreting VMS observationsand gravitational wave source origins.

Enhanced Mass Loss of Very Massive Stars: Impact on the Evolution, Binary Processes, and Remnant Mass Spectrum