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We investigate the formation and evolution of galactic disks immersed inassembling live DM halos. Disk/halo components have been evolved from thecosmological initial conditions and represent the collapse of an isolateddensity perturbation. The baryons include gas (which participates in starformation [SF]) and stars. The feedback from the stellar energy release ontothe ISM has been implemented. We find that (1) The growing triaxial halo figuretumbling is insignificant and the angular momentum (J) is channeled into theinternal circulation; (2) Density response of the disk is out of phase with theDM, thus diluting the inner halo flatness and washing out its prolateness; (3)The total J is neathly conserved, even in models accounting for feedback; (4)The specific J for the DM is nearly constant, while that for baryons isdecreasing; (5) Early stage of disk formation resembles the cat's cradle -- asmall amorphous disk fueled via radial string patterns; (6) The initiallypuffed up gas component in the disk thins when the SF rate drops below ~5Mo/yr; (7) About 40%-60% of the baryons remain outside the SF region; (8)Rotation curves appear to be flat and account for the observed disk/halocontributions; (9) A range of bulge-dominated to bulgeless disks was obtained;Lower density threshold for SF leads to a smaller, thicker disk; Gravitationalsoftening in the gas has a substantial effect on various aspects of galaxyevolution and mimics a number of intrinsic processes within the ISM; (10) Themodels are characterized by an extensive bar-forming activity; (11) Nuclearbars, dynamically coupled and decoupled form in response to the gas inflowalong the primary bars.

Structure Formation Inside Triaxial Dark Matter Halos: Galactic Disks, Bulges and Bars