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Table 1

Fundamental stellar parameters (top) and best-fit values for ΩE and ΩI, without (middle) and with (bottom) a prior on ΩE.

KIC 004914923 KIC 005184732 KIC 006116048 KIC 006933899 KIC 010963065

Teff[K] 5807 ± 89 5744 ± 63 5968 ± 58 5764 ± 46 6158 ± 57
M / M 1.118 ± 0.020 1.205 ± 0.025 1.023 ± 0.021 1.096 ± 0.026 1.062 ± 0.021
R / R 1.378 ± 0.009 1.342 ± 0.010 1.225 ± 0.008 1.574 ± 0.025 1.220 ± 0.009
r cz / R 0.724 0.731 0.757 0.786 0.714
[ Fe / H ] 0.091 ± 0.083 0.384 ± 0.025 − 0.191 ± 0.049 0.126 ± 0.037 − 0.189 ± 0.038
Age [Gyr] 6.23 ± 0.36 4.39 ± 0.13 5.70 ± 0.21 6.57 ± 0.30 4.18 ± 0.19
ΩS [μHz]

Without prior
ΩE [μHz]
ΩI [μHz]
I − ΩE) [μHz]
i [deg]

With prior
ΩE [μHz]
ΩI [μHz]
I − ΩE) [μHz]
I − ΩE) / ΩE
i [deg]

Notes. Top: the effective temperature Teff, mass M, radius R, metallicity [ Fe / H ], age, and radius of the tachocline rcz are derived from stellar structure models. These structure models are obtained from fits to the oscillation mode frequencies and spectroscopic measurements of the effective surface temperature from Bruntt et al. (2012). The surface rotation ΩS is computed from multiple measurements of rotation over the Kepler mission lifetime. All values are adapted from Nielsen et al. (2015). Middle: best-fit values for ΩE, ΩI, and the angle of the stellar inclination angle i, without the application of a prior. Bottom: best-fit values for ΩE, ΩI, and i with the PDF of ΩS used as a prior on ΩE. For all rotation rates and the inclination angle i the errors are given by the 16th and 84th percentile values of the posterior densities of each parameter. For the relative difference between ΩE and ΩI, the average of the percentiles is between − 29% and + 34%, indicating the range of likely configurations of the differential rotation.

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