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We investigate the properties of massive, dense clouds formed in a barredgalaxy and their possible relation to star formation, performing atwo-dimensional hydrodynamical simulation with the gravitational potentialobtained from the 2Mass data from the barred spiral galaxy, M83. Since theenvironment for cloud formation and evolution in the bar region is expected tobe different from that in the spiral arm region, barred galaxies are a goodtarget to study the environmental effects on cloud formation and the subsequentstar formation. Our simulation uses for an initial 80 Myr an isothermal flow ofnon-self gravitating gas in the barred potential, then including radiativecooling, heating and self-gravitation of the gas for the next 40 Myr, duringwhich dense clumps are formed. We identify many cold, dense gas clumps forwhich the mass is more than $10^4M_{\odot}$ (a value corresponding to themolecular clouds) and study the physical properties of these clumps. Therelation of the velocity dispersion of the identified clump's internal motionwith the clump size is similar to that observed in the molecular clouds of ourGalaxy. We find that the virial parameters for clumps in the bar region arelarger than that in the spiral arm region. From our numerical results, weestimate star formation in the bar and spiral arm regions by applying thesimple model of Krumholtz and McKee (2005). The mean relation between starformation rate and gas surface density agrees well with the observedKennicutt-Schmidt relation. The SFE in the bar region is $\sim 60 %$ of thespiral arm region. This trend is consistent with observations of barredgalaxies.

Dense Cloud Formation and Star Formation in a Barred Galaxy