On the origin of the dichotomy of stellar activity cycles

Abstract

The presence of possible correlations between stellar rotation rate $\Omega$ and the frequency of the activity cycle $\omega_\mathrm{cyc}$ is still much debated. We implement a new Bayesian classification algorithm based on a simultaneous regression analysis of multiple scaling laws and we demonstrate the existence of two different scalings in the $\log_{10} \omega_\mathrm{cyc}$ -- $\log_{10} \Omega$ plane for an extended Mt.~Wilson sample of 67 stars. Thanks to metallicity measurements obtained from both ESA Gaia and high-resolution spectroscopy, we argue that the origin of this dichotomy is likely related to the chemical composition: stars whose magnetic cycle frequency increases with rotation rate are less metallic than stars whose magnetic cycle frequency decreases with stellar rotation rates. On the contrary, no clear difference in chromospheric magnetic activity indicators characterizes the two branches.