  In this paper, we explore the evolution of sunspot latitude distribution and
explore its relations with the cycle strength. With the progress of the solar
cycle, the distributions in two hemispheres from mid-latitudes propagate toward
the equator and then (before the usual solar minimum) these two distributions
touch each other. By visualizing the evolution of the distributions in two
hemispheres, we separate the solar cycles by excluding this hemispheric
overlap. From these isolated solar cycles in two hemispheres, we generate
latitude distributions for each cycle, starting from cycle 8 to cycle 23. We
find that the parameters of these distributions, namely, the central latitude
($C$), width ($\delta$) and height ($H$) evolve with the cycle number and they
show some hemispheric asymmetries. Although the asymmetries in these parameters
persist for a few successive cycles, they get corrected within a few cycles and
the new asymmetries appear again. In agreement with the previous study, we find
that distribution parameters are correlated with the strengths of the cycles,
although these correlations are significantly different in two hemispheres. The
general trend that stronger cycles begin sunspot eruptions at relatively higher
latitudes and have wider bands of sunspot emergence latitudes are confirmed
when combining the data from two hemispheres. We explore these features using a
flux transport dynamo model with stochastic fluctuations. We find that these
features are correctly reproduced in this model. The solar cycle evolution of
the distribution center is also in good agreement with observations. Possible
explanations of the observed features based on this dynamo model are presented.
