  We analyzed the sunspot-group daily data that were reported by Greenwich
Photoheliogrphic Results (GPR) during the period 1874-1976 and Debrecen
Photoheliographic Data (DPD) during the period 1977-2017. We determined the
equatorial rotation rate [A] and the latitude gradient [B] components of the
solar differential rotation by fitting the data in each of the 3-year moving
time intervals (3-year MTIs) successively shifted by one year during the period
1874-2017 to the standard law of differential rotation. The values of A and B
around the years of maxima and minima of Solar Cycles 12-24 are obtained from
the 3-year MTIs series of A and B and studied the long-term cycle-to-cycle
modulations in these coefficients. Here we have used the epochs of the maxima
and minima of Solar Cycles 12-24 that were recently determined from the revised
Version-2 international sunspot-number series. We find that there exits a
considerably significant secular decreasing-trend in A around the maxima of
solar cycles. There exist no secular trends in both A and B around the minima
of solar cycles. The secular trend in B around the maxima of solar cycles is
also found to be statistically insignificant. We fitted a cosine function to
the values of A, and also to those of B, after removing the corresponding
linear trends. The cosine-fits suggest that there exist ~54-year (~94-year) and
~82-year (~79-year) periodicities in A (B) around the maxima and minima of
solar cycles, respectively. The amplitude of the cosine-profile of A (B) around
the minima of solar cycles is about 41% (65%) larger than that of A (B) around
the maxima. In addition, the cosine profiles of A and B suggest a large (up to
180 degree) phase difference between the long-term variations of A, and also
between those of B, around maxima and minima of solar cycles.
