  New CCD photometry has been obtained for the RR Lyrae variable star XZ Cygni.
An analysis of old and new photometry confirms earlier results that XZ Cygni
exhibits the Blazhko Effect and that its Blazhko period has changed over time.
These changes in the Blazhko period are anticorrelated with observed changes in
the primary period of XZ Cygni. During the first half of the twentieth century,
XZ Cygni had a Blazhko period of approximately 57.4 d. Beginning in 1965, its
primary period underwent a steep decline in several steps. Coincidentally, its
Blazhko period increased to about 58.5 d. In 1979, the primary period suddenly
increased again. After an interval in which the Blazhko Effect was small, the
Blazhko Effect re-established itself, with a period of approximately 57.5 d.
When its Blazhko period is near 57.5 d, XZ Cygni has also shown a tertiary
period of 41.6 d. We confirm that there is evidence for a longer 3540 d period
in photometry obtained during the first half of the twentieth century. XZ Cygni
is compared with three other RR Lyrae stars which also appear to show changing
Blazhko periods. The observed changes in the length of the Blazhko period of XZ
Cygni constrain possible explanations for the Blazhko Effect. In particular,
they argue against any theoretical explanation which requires that the Blazhko
period be exactly equal to or directly proportional to the rotation period of
the star.
