  The bulk of available stellar activity observations is frequently checked for
the manifestation of signs in comparison with the known characteristic of solar
magnetic modulation. The problem is that stellar activity records are usually
an order of magnitude shorter than available observations of solar activity
variation. Therefore, the resolved time scales of stellar activity are
insufficient to decide reliably that a cyclic variation for a particular star
is similar to the well-known 11-yr sunspot cycles. As a result, recent studies
report several stars with double or multiple cycles which serve to challenge
the underlying theoretical understanding. This is why a consistent method to
separate 'true' cycles from stochastic variations is required. In this paper,
we suggest that a conservative method, based on the best practice of wavelet
analysis previously applied to the study of solar activity, for studying and
interpreting the longest available stellar activity record - photometric
monitoring of V833 Tau for more than 100 years. We find that the observed
variations of V833 Tau with timescales of 2-50 yr should be comparable with the
known quasi-periodic solar mid-term variations, whereas the true cycle of V833
Tau, if it exists, should be of about a century or even longer. We argue that
this conclusion does not contradict the expectations from stellar dynamo
theory.
