In Auriga simulations, boxy/peanut bulges form 1.1-1.6 Gyr after bar formation, always after a buckling event, and appear in 45% of barred galaxies at z=0, dropping to zero by z~1.
Formation and evolution of bulges
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abstract
After presenting three ways of defining a bulge component in disc galaxies, we introduce the various types of bulges, namely the classical bulges, the boxy/peanut bulges and the disc-like bulges. We then discuss three specific topics linked to bulge formation and evolution, namely the coupled time evolution of the bar, buckling and peanut strengths; the effect of velocity anisotropy on peanut formation; and bulge formation via bar destruction.
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Formation and evolution of boxy/peanut bulges in the Auriga cosmological simulations
In Auriga simulations, boxy/peanut bulges form 1.1-1.6 Gyr after bar formation, always after a buckling event, and appear in 45% of barred galaxies at z=0, dropping to zero by z~1.