  Using N-body simulations we explore the effects of growing a supermassive
black hole (SMBH) prior to or during the formation of a stellar bar. Keeping
the final mass and growth rate of the SMBH fixed, we show that if it is
introduced before or while the bar is still growing, the SMBH does not cause a
decrease in bar amplitude. Rather, in most cases, it is strengthened. In
addition early growing SMBHs always either decreases the buckling amplitude,
delay buckling, or both. This weakening of buckling is caused by an increase in
the disk vertical velocity dispersion at radii well beyond the nominal black
hole sphere-of-influence. While we find considerable stochasticity and
sensitivity to initial conditions, the only case where the SMBH causes a
decrease in bar amplitude is when it is introduced after the bar has attained a
steady state. In this case we confirm previous findings that the decrease in
bar strength is a result of scattering of bar-supporting orbits with small
pericenter radii. By heating the inner disk both radially and vertically, an
early growing SMBH increases the fraction of stars that can be captured by the
Inner Lindblad Resonance (ILR) and the vertical ILR, thereby strengthening both
the bar and the boxy peanut shaped bulge. Using orbital frequency analysis of
star particles, we show that when an SMBH is introduced early and the bar forms
around it, the bar is populated by different families of regular bar-supporting
orbits than when the bar forms without an SMBH.
