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We use high resolution numerical simulations in order to analyze the stellarbar evolution in spinning dark matter (DM) halos. Previous works have shownthat the halo spin has a substantial effect on the bar evolution and can leadto bar dissolution following the vertical buckling instability. Here, we invokethe DM spin sequence, $\lambda=0-0.09$, and study the effect of DM densityalong this $\lambda$-sequence by varying the compactness of DM halo. We findthat (1) varying the DM density has a profound effect on the stellar barevolution along the $\lambda$-sequence, namely, on its amplitude, patternspeed, buckling time, etc.; (2) For $\lambda\gtrsim 0.04$, the bucklinginstability has been delayed progressively, and does not occur when the bar hasreached its maximal strength; (3) Instead, stellar bars remain near maximalstrength, and their amplitude plateau stage extends over $\sim 1-7$ Gyr,terminating with the buckling instability; (4) Although stellar bars remainstrong during the plateau, their pattern speed stays nearly constant. Thereason for this unusual behavior of stellar bars follows from the highlyreduced gravitational torques which they experience due to the DM bar beingaligned with the stellar bar. The performed orbital analysis shows that thedelayed buckling results from a slow evolution of stellar oscillations alongthe bar major and vertical axes -- thus postponing the action of the vertical2:1 resonance which pumps the rotational energy into vertical motions; (5)Peanut/boxy shaped bulges form at the beginning of the plateau and grow withtime; (6) Strong stellar bars in spinning halos can avoid fast braking,resolving the long standing discrepancy between observations and $N$-bodysimulations. This behavior of stellar bars along the $\lambda$- and DMdensity-sequences, reveals a wealth of stellar bar properties which requireadditional study.

Stellar Bars in Spinning Halos: Delayed Buckling and Absence of Slowdown