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tokens: Distribution parameters, namely , and δ , show significant positive correlations with the cycle strengths. These correlations are in general agreement with the previous findings of Solanki et al. ( 2008 ), although there are some differences in the values of the correlations, as the cycle lengths are computed differently in their study. In general, the observed correlations imply that stronger cycles begin sunspot eruptions at relatively higher latitudes, and they have wider extends of sunspot eruption latitudes. Another interesting result from this study is the hemispheric asymmetry in the distribution parameters, especially in the center values ( C ). We find that the parameter oscillates around the zero value, whereas the amplitude of this oscillation seems to decrease with the increase of the cycle number. To explore these features, we have applied a flux transport dynamo model in which polar field at the solar minimum is varied randomly. Although this model produces many features of the solar cycle correctly, the latitudinal distribution of sunspots is not in good agreement with observation because of the fewer sunspots near the equator. Despite of this dissimilarity, all correlations among the distribution parameters, as obtained in observation, are reproduced correctly. Our results are in broad agreement with that of Solanki et al. ( 2008 ), who reproduced similar correlations using a simplified thin shell dynamo model. While our model has a fixed single-cell (in each hemisphere) meridional flow, Solanki et al. ( 2008 ) showed that the model with and without meridional flow produce slightly different results. Our model also reproduces the detailed variation of these parameters within the cycle, as demonstrated by Cameron Schüssler ( 2016 ). Thus, our study supports a considerable variation in the polar field as the cause of the irregular solar cycle and variations in the latitude distributions. The variation in the polar field is directly and indirectly observed in the Sun (Muñoz-Jaramillo et al. 2013 ; Priyal et al. 2014 ). This variation is primarily caused by the the scatter in the tilt angles of active regions around Joy’s law (Cameron et al. 2013 ; Jiang et al. 2014 ; Hazra et al. 2017 ; Karak Miesch 2017 ), which is actually observed in the Sun (e.g., Dasi-Espuig et al. 2010 ; Stenflo Kosovichev 2012 ). While it is known that the variation in the meridional flow is expected to cause some variations in the solar cycle (e.g., Karak Choudhuri 2011 ; Belucz Dikpati 2013 ), due to difficulties in the measurements, we are uncertain about the amount of variation present in the deep meridional flow. However, the surface meridional flow is observed to change with the solar cycle and most of this variation is probably caused by the inflows around the active regions (Gizon et al. 2010 ). This meridional flow perturbation can change the polar field from cycle to cycle (Jiang et al. 2010 ; Hathaway Upton 2014 ; Shetye et al. 2015 ). In our