A study of convective core overshooting as a function of stellar mass based on two-dimensional hydrodynamical simulations

We perform two-dimensional numerical simulations of core convection for zero-age-main-sequence stars covering a mass range from 3 $M_\odot$ to 20 $M_\odot$. The are performed with the fully compressible time-implicit code MUSIC. study efficiency overshooting, which describes ballistic process convective flows crossing boundary, as function stellar and luminosity. also impact artificially increasing luminosity models. cover hundreds thousands turnover timescales. Applying framework extreme plume events previously developed envelopes, we derive overshooting lengths masses. find that distance ($d_{\rm ov}$) scales ($L$) radius ($r_{\rm conv}$). scaling law $d_{\rm ov} \propto L^{1/3} r_{\rm conv}^{1/2}$ is implemented in 1D evolution resulting models compared observations. predicts values significantly increase mass, qualitative agreement Quantitatively, however, predicted underestimated masses $\gtrsim 10 M_\odot$. Our 2D show formation nearly-adiabatic layer just above Schwarzschild boundary core, exhibited recent 3D convection. most luminous growth size time layer. This seems slow down upper edge gets closer maximum length simulation exceeds typical thermal diffusive timescale