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Context: The internal characteristics of stars, such as their core rotationrates, are obtained via asteroseismic observations. A comparison of corerotation rates found in this way with core rotation rates as predicted bystellar evolution models demonstrate a large discrepancy. This means that theremust be a process of angular momentum transport missing in the current theoryof stellar evolution. A new formalism was recently proposed to fill in for thismissing process, which has the Tayler instability as its starting point(hereafter referred to as `Fuller-formalism'). Aims: We investigate the effectof the Fuller-formalism on the internal rotation of stellar models with aninitial mass of 2.5 Mo. Methods: Stellar evolution models, including theFuller-formalism, of intermediate-mass stars were calculated to make acomparison between asteroseismically obtained core rotation rates in the coreHe burning phase and in the white dwarf phase. Results: Our main results showthat models including the Fuller-formalism can match the core rotation ratesobtained for the core He burning phases. However, these models are unable tomatch the rotation rates obtained for white dwarfs. When we exclude theFuller-formalism at the end of the core He burning phase, the white dwarfrotation rates of the models match the observed rates. Conclusions: We concludethat in the present form, the Fuller-formalism cannot be the sole solution forthe missing process of angular momentum transport in intermediate-mass stars.

astronomy and astrophysics

Asteroseismology of evolved stars to constrain the internal transport of  angular momentum. III. Using the rotation rates of intermediate-mass stars to  test the Fuller-formalism