We analyzed the host stars of the present sample of confirmed planets detected by Kepler and Kepler Objects of Interest ( KOI ) to compute new photometric rotation periods and to study the behavior of their angular momentum .
Lomb–Scargle periodograms and wavelet maps were computed for 3 , 807 stars .
For 540 of these stars , we were able to detect rotational modulation of the light curves at a significance level of greater than 99 % .
For 63 of these 540 stars , no rotation measurements were previously available in the literature .
According to the published masses and evolutionary tracks of the stars in this sample , the sample is composed of M– to F–type stars ( with masses of 0.48–1.53 M _ { \sun } ) with rotation periods that span a range of 2 to 89 days .
These periods exhibit an excellent agreement with previously reported ( for the stars for which such values are available ) , and the observed rotational period distribution strongly agrees with theoretical predictions .
Furthermore , for the 540 sources considered here , the stellar angular momentum provides an important test of Kraft ’ s relation based on the photometric rotation periods .
Finally , this study directly contributes in a direct approach to our understanding of how angular momentum is distributed between the host star and its ( detected ) planetary system ; the role of angular momentum exchange in such systems is an unavoidable piece of the stellar rotation puzzle .