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We study the effect of large-scale magnetic fields on the non-axisymmetricRossby wave instability (RWI) in accretion discs. The instability developsaround a density bump, which is likely present in the transition region betweenthe active zone and dead zone of protoplanetary discs. Previous works suggestthat the vortices resulting from the RWI may facilitate planetesimal formationand angular momentum transport. We consider discs threaded by a large-scalepoloidal magnetic field, with a radial field component at the disc surface.Such field configurations may lead to the production of magnetic winds or jets.In general, the magnetic field can affect the RWI even when it is sub-thermal(plasma $\beta\sim 10$). For infinitely thin discs, the instability can beenhanced by about 10 percent. For discs with finite thickness, with a radialgradient of the magnetic field strength, the RWI growth rate can increasesignificantly (by a factor of $\sim 2$) as the field approaches equipartition($\beta \sim 1$). Our result suggests that the RWI can continue to operate indiscs that produce magnetic winds.

Rossby Wave Instability in Accretion Discs with Large-Scale Poloidal Magnetic Fields