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The physical mechanisms driving the transport of angular momentum in starsare not fully understood, as current models cannot explain the observed stellarrotation profiles across all stages of evolution. By making use of pulsatingF-type dwarfs, this work aims at (i) observationally calibrating the efficiencyof angular momentum transport, assuming a constant uniform viscosity, and (ii)testing how well state-of-the-art rotating stellar models with angular momentum(AM) transport by rotationally-induced processes can explain observed rotationprofiles. In both cases, the aim is to simultaneously reproduce the measurednear-core rotation and core-to-surface rotation ratio. Asteroseismic modellingis applied to a sample of seven slowly rotating pulsators, to derive (core)masses and ages from their gravity-mode oscillations. This work focuses on themain sequence, using models that start with an initial uniform rotationfrequency at the start of core-hydrogen burning that is a free parameter. Twotreatments of AM transport are considered: (i) a constant uniform viscosity,and (ii) rotationally-induced processes. Next, the initial rotation frequencyof each star is derived from the observed present-day near-core rotationfrequency for both treatments. To explain the near-core rotation rate at theinferred age, initial rotation frequencies at the zero-age main sequence needto be below 10 percent of the initial critical break-up frequency. A diffusiveapproximation of angular momentum transport can in general explain the observedrotation profiles of the six slowly-rotating F-type dwarfs, for average valuesof the viscosity between 2x10^5 and 5x10^7 cm^2/s or when the viscosity iscomputed from rotationally-induced mechanisms. Yet, for three stars in thesample, the core-to-surface rotation fraction from rotationally-inducedmechanisms is predicted to be higher than observed.

Calibrating angular momentum transport in intermediate-mass stars from gravity-mode asteroseismology