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We investigate whether the elliptical instability is important for tidaldissipation in gaseous planets and stars. In a companion paper, we found thatthe conventional elliptical instability results in insufficient dissipationbecause it produces long-lived vortices that then quench further instability.Here, we study whether the addition of a magnetic field prevents those vorticesfrom forming, and hence leads to enhanced dissipation. We present results frommagnetohydrodynamical simulations that evolve the elliptical instability in alocal patch of a rotating planet or star, in the presence of a weak magneticfield. We find that magnetic fields do indeed prevent vortices from forming,and hence greatly enhance the steady state dissipation rate. In addition, theresulting turbulence acts as a small-scale dynamo, amplifying the initiallyweak field. The inferred tidal dissipation is potentially important at shortorbital periods. For example, it can circularise hot Jupiters with orbitalperiods shorter than 2.5 days, and synchronise their spins with their orbitsout to 6 days. However, it appears unable to account for the hot Jupiters thatappear to have been circularised out to six to ten day orbital periods. It alsocannot account for the inferred circularisation of many close binary stars.

Nonlinear evolution of the elliptical instability in the presence of weak magnetic fields