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The merger of a white dwarf (WD) and a neutron star (NS) is a relativelycommon event that will produce an observable electromagnetic signal.Furthermore, the compactness of these stellar objects makes them an interestingcandidate for gravitational wave (GW) astronomy, potentially being in thefrequency range of LISA and other missions. To date, three-dimensionalsimulations of these mergers have not fully modelled the WD disruption, or haveused lower resolutions and have not included magnetic fields even though theypotentially shape the evolution of the merger remnant. In this work, wesimulate the merger of a 1.4$M_\odot$ NS with a 1$M_\odot$ carbon oxygen WD inthe magnetohydrodynamic moving mesh code \AREPO. We find that the disruption ofthe WD forms an accretion disk around the NS, and the subsequent accretion bythe NS powers the launch of strongly magnetized, mildly relativistic jetsperpendicular to the orbital plane. Although the exact properties of the jetscould be altered by unresolved physics around the NS, the event could result ina transient with a larger luminosity than kilonovae. We discuss possibleconnections to fast blue optical transients (FBOTs) and long-duration gamma-raybursts. We find that the frequency of GWs released during the merger is toohigh to be detectable by the LISA mission, but suitable for deci-hertzobservatories such as LGWA, BBO or DECIGO.

Self-consistent MHD simulation of jet launching in a neutron star - white dwarf merger