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We investigate the dependence of occurrence of bars in galaxies on galaxyproperties and environment. We use a volume-limited sample of 33,391 galaxiesbrighter than $M_{r}=-19.5+5$log$h$ at $0.02\le z\le0.05489$, drawn from theSDSS DR 7. We classify the galaxies into early and late types, and identifybars by visual inspection. Among 10,674 late-type galaxies with axis ratio$b/a>0.60$, we find 3,240 barred galaxies ($f_{bar}=30.4%$) which divide into2,542 strong bars ($f_{SB1}=23.8%$) and 698 weak bars ($f_{SB2}=6.5%$). We findthat $f_{SB1}$ increases as $u-r$ color becomes redder, and that it has amaximum value at intermediate velocity dispersion ($\sigma\simeq$150 kms$^{-1}$). This trend suggests that strong bars are dominantly hosted byintermediate-mass systems. Weak bars prefer bluer galaxies with lower mass andlower concentration. In the case of strong bars, their dependence on theconcentration index appears only for massive galaxies with $\sigma>150$ kms$^{-1}$. We also find that $f_{bar}$ does not directly depend on thelarge-scale background density when other physical parameters ($u-r$ color or$\sigma$) are fixed. We discover that $f_{SB1}$ decreases as the separation tothe nearest neighbor galaxy becomes smaller than 0.1 times the virial radius ofthe neighbor regardless of neighbor's morphology. These results imply thatstrong bars are likely to be destroyed during strong tidal interactions, andthat the mechanism for this phenomenon is gravitational and not hydrodynamical.The fraction of weak bars has no correlation with environmental parameters. Wedo not find any direct evidence for environmental stimulation of bar formation.

Dependence of Barred Galaxy Fraction on Galaxy Properties and Environment