  The distribution of the stellar rotation axes of 113 main sequence stars in
the open cluster Praesepe are examined by using current photometric rotation
periods, spectroscopic rotation velocities, and estimated stellar radii. Three
different samples of stellar rotation data on spotted stars from the Galactic
field and two independent samples of planetary hosts are used as control
samples to support the consistency of the analysis. Considering the high
completeness of the Praesepe sample and the behavior of the control samples, we
find that the main sequence F - K stars in this cluster are susceptible to
rotational axis alignment. Using a cone model, the most likely inclination
angle is 76+/-14 degrees with a half opening angle of 47+/-24 degrees.
Non-isotropic distribution of the inclination angles is preferred over the
isotropic distribution, except if the rotation velocities used in this work are
systematically overestimated. We found no indication of this being the case on
the basis of the currently available data.
