  The merger of a white dwarf (WD) and a neutron star (NS) is a relatively
common event that will produce an observable electromagnetic signal.
Furthermore, the compactness of these stellar objects makes them an interesting
candidate for gravitational wave (GW) astronomy, potentially being in the
frequency range of LISA and other missions. To date, three-dimensional
simulations of these mergers have not fully modelled the WD disruption, or have
used lower resolutions and have not included magnetic fields even though they
potentially shape the evolution of the merger remnant. In this work, we
simulate the merger of a 1.4$M_\odot$ NS with a 1$M_\odot$ carbon oxygen WD in
the magnetohydrodynamic moving mesh code \AREPO. We find that the disruption of
the WD forms an accretion disk around the NS, and the subsequent accretion by
the NS powers the launch of strongly magnetized, mildly relativistic jets
perpendicular to the orbital plane. Although the exact properties of the jets
could be altered by unresolved physics around the NS, the event could result in
a transient with a larger luminosity than kilonovae. We discuss possible
connections to fast blue optical transients (FBOTs) and long-duration gamma-ray
bursts. We find that the frequency of GWs released during the merger is too
high to be detectable by the LISA mission, but suitable for deci-hertz
observatories such as LGWA, BBO or DECIGO.
