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Barred structures are widespread in a considerable fraction of galacticdiscs, spanning diverse environments and galaxy luminosities. The environmentlikely exerts a significant influence on bar formation. It is plausible thatthe structural parameters of bars resulting from tidal interactions inhigh-density galactic environments differ from those formed through internaldisc instabilities in isolated galaxies. To empirically test this scenario, aviable approach is to compare the structural parameters of bars in galaxiessituated within distinct environments. We have collected data on the bar radiusand bar strength for a sample of 36 SB0 and SBa galaxies located within theVirgo cluster. Additionally, we analyzed a sample of 46 field galaxies withsimilar morphologies and luminosity range. The analysis reveals that the barradius exhibits a correlation with galaxy luminosity, indicating that largerbars are typically found in more luminous galaxies. When comparing galaxieswith fixed luminosities, the field galaxies display larger bar radii comparedto those in the Virgo cluster. However, when the bar radius is scaled by thesize of the galaxy, the disparity diminishes and the scaled bars in the Virgocluster and the field exhibit similar sizes. This is because galaxies ofsimilar luminosities tend to be larger in the field environment compared to thecluster and because the bars adapt to the discs in which they live. Regardingthe bar strength, no significant differences were observed for bright galaxies($M_{r} < -19.5$) between those located in the Virgo cluster and those in thefield. In contrast, faint galaxies ($M_{r} > -19.5$) show stronger bars in thefield than in the cluster.

Properties of Barred Galaxies with the Environment: I. the case of the Virgo cluster