  Stellar bars and spiral arms co-exist and co-evolve in most disc galaxies in
the local Universe. However, the physical nature of this interaction remains a
matter of debate. In this work, we present a set of numerical simulations based
on isolated galactic models aimed to explore how the bar properties affect the
induced spiral structure. We cover a large combination of bar properties,
including the bar length, axial ratio, mass and rotation rate. We use three
galactic models describing galaxies with rising, flat and declining rotation
curves. We found that the pitch angle best correlates with the bar pattern
speed and the spiral amplitude with the bar quadrupole moment. Our results
suggest that galaxies with declining rotation curves are the most efficient
forming grand design spiral structure, evidenced by spirals with larger
amplitude and pitch angle. We also test the effects of the velocity ellipsoid
in a subset of simulations. We found that as we increase the radial anisotropy,
spirals increase their pitch angle but become less coherent with smaller
amplitude.
