The Radiative–Convective Gap: Fact or Fiction?

Abstract Gaia characterizes the stellar populations of nearby open clusters with unprecedented precision. We investigate the Böhm-Vitense gap, which has been found as a prominent feature in the stellar sequence of open clusters. Using PARSEC isochrone fitting, we derive astrophysical parameters for more than 1100 bona fide single stars each in Praesepe, identify more than 1100 bona fide single stars in the α Persei (Melotte 20) open cluster, and confirm their approximate match in terms of age (≈710 and ≈45 Myr) and metallicity ([M/H] ≈ +0.15 and ≈+0.13 dex) to the Hyades and Pleiades, respectively. By merging data of the cluster pairs, we improve number statistics. We do not find a clear gap in the combined observational G abs versus BP − RP color–magnitude diagram (CMD) in the stellar mass range corresponding to the location of the Böhm-Vitense gap. We reproduce gaps in simulated Hyades-type CMDs randomly drawn from an initial mass function. There is no strong evidence for a discontinuity originating in the transition from radiative to convective energy transport in the stellar photosphere. We conclude that the observed gaps in the stellar sequences of open clusters could be explained by small number statistics and the uneven mass–color relation at the transition from spectral type A to F.