We analyze K2 light curves for 132 low-mass ( 1 { \lower 3.44 pt \hbox { $ \buildrel > \over { \sim } $ } } M _ { * } { \lower 3.44 pt \hbox { $% \buildrel > \over { \sim } $ } } 0.1 { M _ { \odot } } ) members of the 600–800 Myr-old Hyades cluster and measure rotation periods ( P _ { rot } ) for 116 of these stars .
These include 93 stars with no prior P _ { rot } measurement ; the total number of Hyads with known P _ { rot } is now 232 .
We then combine literature binary data with Gaia DR2 photometry and astrometry to select single star sequences in the Hyades and its roughly coeval Praesepe open cluster , and derive a new reddening value of A _ { V } = 0.035 \pm 0.011 for Praesepe .
Comparing the effective temperature– P _ { rot } distributions for the Hyades and Praesepe , we find that solar-type Hyads rotate , on average , 0.4 d slower than their Praesepe counterparts .
This P _ { rot } difference indicates that the Hyades is slightly older than Praesepe : we apply a new gyrochronology model tuned with Praesepe and the Sun , and find an age difference between the two clusters of 57 Myr .
However , this P _ { rot } difference decreases and eventually disappears for lower-mass stars .
This provides further evidence for stalling in the rotational evolution of these stars , and highlights the need for more detailed analysis of angular-momentum evolution for stars of different masses and ages .