![Photometric magnetic activity index, Sph, as a function of the Rossby for the Kepler stars Photometric magnetic activity index, Sph, as a function of the Rossby for the Kepler stars showing the comparison between an older relation to compute the Rossby number (left panel, Noyes 1984) and the Rossby number from this work (right panel).](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/Ro_LEGACY.png?h=bfb5739d&itok=ihMgs0Qc)
In a star like the Sun, surface magnetic activity results from the interaction between rotation, convection, and magnetic field. One of the key parameters to study the magnetic activity of stars is the Rossby number, which is the ratio between the surface rotation period of the star and the convective turnover time. The convective turnover time measures the time that takes a bubble of plasma to go from the base of the convective zone in a star like the Sun to the surface, similarly to a bubble reaching the surface in a pan with boiling water heated by the bottom. While the surface rotation
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