Abstract
The measurements performed in Chaps. 3 and 4 can be used to make more quantitative statements about the internal rotation profile of the studied stars. We determined that the difference in the rotational splittings as a function of frequency is not large, consistent with what would be observed in the Sun if viewed as a star. In addition to this we found that the spot rotation periods are consistent with the seismic rotation periods; showing that any radial or latitudinal differential rotation is likely small. In this section we will use forward modeling with a simple radial step rotation profile and investigate how well the above mentioned measurements can constrain such a model. This will allow us to estimate the upper limits of the radial shear at the tachocline.
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Nielsen, M.B. (2017). Discussion: Constraining Interior Rotational Shear. In: Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-50989-1_5
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