Table 3
Slow-down rates on the RGB.
| Variable | a2012,now | aus |
|---|---|---|
| R∕R⊙ | − 0.38 ± 0.15 | − 0.17 ± 0.19 |
 |
− 0.13 ± 0.07 | − 0.10 ± 0.09 |
Notes. Fit of the core rotational splitting is a function of either the stellar radius or the mixed-mode density. These fits are based on stars that are common to our study and to that of Mosser et al. (2012b). The values taken by a2012,now are derived from Mosser et al. (2012b) measurements while aus values are derived from our measurements.
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