Convective core overshooting has a strong influence on the evolution of stars of moderate and high mass .
Studies of double-lined eclipsing binaries and stellar oscillations have renewed interest in the possible dependence of overshooting on stellar mass , which has been poorly constrained by observations so far .
Here we have used a sample of 29 well-studied double-lined eclipsing binaries in key locations of the H-R diagram to establish the explicit dependence of f _ { ov } on mass , where f _ { ov } is the free parameter in the diffusive approximation to overshooting .
Measurements of the masses , radii , and temperatures of the binary components were compared against stellar evolution calculations based on the MESA code to infer semi-empirical values of f _ { ov } for each component .
We find a clear mass dependence such that f _ { ov } rises sharply from zero in the range 1.2– 2.0 ~ { } M _ { \sun } , and levels off thereafter up to the 4.4 M _ { \sun } limit of our sample .
Tests with two different element mixtures indicate the trend is the same , and we find it is also qualitatively similar to the one established in our previous study with the classical step-function implementation of overshooting characterized by the free parameter \alpha _ { ov } .
Based on these measurements we infer an approximate relationship between the two overshooting parameters of { \alpha _ { ov } } / { f _ { ov } } = 11.36 \pm 0.22 , with a possible dependence on stellar properties .