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The importance of the existence of a radiative core in generating asolar-like magnetic dynamo is still unclear. Analytic models andmagnetohydrodynamic simulations of stars suggest the thin layer between astar's radiative core and its convective zone can produce shearing thatreproduces key characteristics of a solar-like dynamo. However, recent studiessuggest fully and partially convective stars exhibit very similarperiod-activity relations, hinting that dynamos generated by stars with andwithout radiative cores hold similar properties. Here, using kinematic ages, wediscover an abrupt change in the stellar spin-down law across the fullyconvective boundary. We found that fully convective stars exhibit a higherangular momentum loss rate, corresponding to a torque that is $\sim$ 2.25 timeshigher for a given angular velocity than partially convective stars around thefully convective boundary. This requires a dipole field strength that is largerby a factor of $\sim$2.5, a mass loss rate that is $\sim$4.2 times larger, orsome combination of both of those factors. Since stellar-wind torques dependprimarily on large-scale magnetic fields and mass loss rates, both of whichderive from magnetic activity, the observed abrupt change in spin-down lawsuggests that the dynamos of partially and fully convective stars may befundamentally different

An abrupt change in the stellar spin-down law at the fully convective boundary