2017ApJ...849...18C

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_☉, and levels off thereafter up to the 4.4 M_☉ limit of our sample. Tests with two different element mixtures indicate the trend is the same, and we find it to also be qualitatively similar to the one established in our previous study with the classical step-function implementation of overshooting characterized by the free parameter α_ov. Based on these measurements, we infer an approximate relationship between the two overshooting parameters of α_ov/f_ov=11.36±0.22, with a possible dependence on stellar properties.