L. M. Rebull, J. R. Stauffer, J. Bouvier, A. M. Cody, L. A. Hillenbrand, D. R. Soderblom, J. Valenti, D. Barrado, H. Bouy, D. Ciardi, M. Pinsonneault, K. Stassun, G. Micela, S. Aigrain, F. Vrba, G. Somers, E. Gillen, A. Collier Cameron. 2016. Rotation in the Pleiades with K2: II. Multi-Period Stars. Astronomical Journal 152, 5, DOI: 10.3847/0004-6256/152/5/114
We use K2 to continue the exploration of the distribution of rotation periods in Pleiades that we began in Paper I. We have discovered complicated multiperiod behavior in Pleiades stars using these K2 data, and we have grouped them into categories, which are the focal part of this paper. About 24% of the sample has multiple, real frequencies in the periodogram, sometimes manifesting as obvious beating in the LCs. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P versus. (V – K-s)(0) identified in Paper I. The fast sequence in P versus. (V – K-s)(0) is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.
