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By means of the data sets of the Panoramic Survey Telescope and RapidResponse System (Pan-STARRS), we investigate the relationship between thevariability amplitude and luminosity at 5100 \AA, black hole mass, Eddingtonratio, $ R_{\rm Fe \, II}$ ( the ratio of the flux of Fe II line within4435-4685 \AA ~to the broad proportion of $\rm H\beta$ line) as well as $R_{5007}$ (the ratio of the flux [O III] line to the total $\rm H\beta$ line)of the broad line Seyfert 1 (BLS1) and narrow line Seyfert 1 (NLS1) galaxiessample in g,r,i,z and y bands, respectively. We also analyze the similaritiesand differences of the variability characteristics between the BLS1 galaxiesand NLS1 galaxies. The results are listed as follows. (1). The cumulativeprobability distribution of the variability amplitude shows that NLS1 galaxiesare lower than that in BLS1 galaxies. (2). We analyze the dependence of thevariability amplitude with the luminosity at 5100 \AA, black hole mass,Eddington ratio, $ R_{\rm Fe \,II}$ and $ R_{5007}$, respectively. We findsignificantly negative correlations between the variability amplitude andEddington ratio, insignificant correlations with the luminosity at 5100 \AA.The results also show significantly positive correlations with the black holemass and $ R_{5007}$, significantly negative correlations with $ R_{\rm Fe\,II}$ which are consistent with Rakshit and Stalin(2017) in low redshift bins(z<0.4) and Ai et al.(2010). (3). The relationship between the variabilityamplitude and the radio loudness is investigated for 155 BLS1 galaxies and 188NLS1 galaxies. No significant correlations are found in our results.

The comparison of optical variability of broad-line Seyfert 1 and narrow-line Seyfert 1 galaxies from the view of Pan-STARRS