This is the third of a series of papers presenting the first attempt toanalyze the growth of the bar instability in a consistent cosmologicalscenario. In the previous two articles we explored the role of the cosmology onstellar disks, and the impact of the gaseous component on a disk embedded in acosmological dark matter halo. The aim of this paper is to point out the impactof the star formation on the bar instability inside disks having different gasfractions. We perform cosmological simulations of the same disk-to-halo masssystems as in the previous works where the star formation was not triggered. Wecompare the results of the new simulations with the previous ones toinvestigate the effect of the star formation by analysing the morphology of thestellar components, the bar strength, the behaviour of the pattern speed. Wefollow the gas and the central mass concentration during the evolution andtheir impact on the bar strength. In all our cosmological simulations a stellarbar, lasting 10 Gyr, is still living at z=0. The central mass concentration ofgas and of the new stars has a mild action on the ellipticity of the bar but isnot able to destroy it; at z=0 the stellar bar strength is enhanced by the starformation. The bar pattern speed is decreasing with the disk evolution.
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