  Bar driven secular evolution plays a key role in changing the morphology and
kinematics of disk galaxies, leading to the formation of rapidly rotating
boxy/peanut bulges. If these disk galaxies also hosted a preexisting classical
bulge, how would the secular evolution influence the classical bulge, and also
the observational properties.
  We first study the co-evolution of a bar and a preexisting non-rotating
low-mass classical bulge such as might be present in galaxies like the Milky
Way. It is shown with N-body simulations that during the secular evolution,
such a bulge can gain significant angular momentum emitted by the bar through
resonant and stochastic orbits. Thereby it transforms into a cylindrically
rotating, anisotropic and triaxial object, embedded in the fast rotating boxy
bulge that forms via disk instability (Saha et al. 2012). The composite
boxy/peanut bulge also rotates cylindrically.
  We then show that the growth of the bar depends only slightly on the rotation
properties of the preexisting classical bulge. For the initially rotating small
classical bulge, cylindrical rotation in the resulting composite boxy/peanut
bulge extends to lower heights (Saha & Gerhard 2012). More massive classical
bulges also gain angular momentum emitted by the bar, inducing surprisingly
large rotational support within about 4 Gyrs (Saha et al. in prep).
