  We study how bar strength and bar kinematics affect star formation in
different regions of the bar by creating radial profiles of EW[H$\alpha$] and
D$_{\rm n}$4000 using data from SDSS-IV MaNGA. Bars in galaxies are classified
as strong or weak using Galaxy Zoo DESI, and they are classified as fast and
slow bars using the Tremaine-Weinberg method on stellar kinematic data from the
MaNGA survey. In agreement with previous studies, we find that strong bars in
star forming galaxies have enhanced star formation in their centre and beyond
the bar-end region, while star formation is suppressed in the arms of the bar.
This is not found for weakly barred galaxies, which have very similar radial
profiles to unbarred galaxies. In addition, we find that slow bars in star
forming galaxies have significantly higher star formation along the bar than
fast bars. However, the global star formation rate is not significantly
different between galaxies with fast and slow bars. This suggests that the
kinematics of the bar do not affect star formation globally, but changes where
star formation occurs in the galaxy. Thus, we find that a bar will influence
its host the most if it is both strong and slow.
