Bulges or Bars from Secular Evolution?

We use high resolution collisionless $N$-body simulations to study thesecular evolution of disk galaxies and in particular the final properties ofdisks that suffer a bar and perhaps a bar-buckling instability. Although wefind that bars are not destroyed by the buckling instability, when we decomposethe radial density profiles of the secularly-evolved disks into inner S\'ersicand outer exponential components, for favorable viewing angles, the resultingstructural parameters, scaling relations and global kinematics of the barcomponents are in good agreement with those obtained for bulges of late-typegalaxies. Round bulges may require a different formation channel ordissipational processes.Comment: Accepted to ApJL. 4 figures, 2 in color Corrected minor typos and reference lis