A synthetic population of Wolf-Rayet stars in the LMC based on detailed single and binary star evolution models

Without doubt, mass transfer in close binary systems contributes to the populations of Wolf-Rayet (WR) stars Milky Way and Magellanic Clouds. However, formation channel is so far not well explored. We want remedy this by exploring large grids detailed single star evolution models computed with publicly available MESA code, for a metallicity appropriate Large Cloud (LMC). The are calculated through Roche-lobe overflow transfer, until initially more massive exhausts helium its core. distinguish WR based on estimated stellar wind optical depth. use these build synthetic population, assuming constant formation. Our can reproduce population LMC significant detail, including number luminosity functions main subtypes. find that fractions 100% (50%), all below $10^6\,L_{\odot}$ ($10^{5.7}\,L_{\odot}$) stripped donors. also identify several insightful mismatches. With fraction 50\%, our produce too many yellow supergiants, calling either larger initial fraction, or enhanced mass-loss near Humphreys-Davidson limit. predict long-period binaries than observed, arguably due an observational bias towards short periods. underpredict shortest-period binaries, which may have implications understanding progenitors double black hole mergers. produced be often assumed, outline risk mis-calibrate physics when only used observed stars.