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We report results from general relativistic radiation MHD (GRRMHD)simulations of a super-Eddington black hole (BH) accretion disk formed as aresult of a tidal disruption event (TDE). We consider the fiducial case of asolar mass star on a mildly penetrating orbit disrupted by a supermassive BH ofmass $10^6 \, M_\odot$, and consider the epoch of peak fall back rate. Wepost-process the simulation data to compute viewing angle dependent spectra. Weperform a parameter study of the dynamics of the accretion disk as a functionof BH spin and magnetic flux, and compute model spectra as a function of theviewing angle of the observer. We also consider detection limits based on themodel spectra. We find that an accretion disk with a relatively weak magneticfield around the BH (so-called SANE regime of accretion) does not launch arelativistic jet, whether or not the BH is rotating. Such models reasonablyreproduce several observational properties of non-jetted TDEs. The same is alsotrue for a non-rotating BH with a strong magnetic field (MAD regime). One ofour simulations has a rapidly rotating BH (spin parameter 0.9) as well as a MADaccretion disk. This model launches a powerful relativistic jet, which ispowered by the BH spin energy. It reproduces the high energy emission and jetstructure of the jetted TDE Swift J1644+57 surprisingly well. Jetted TDEs maythus correspond to the subset of TDE systems that have both a rapidly spinningBH and MAD accretion.

GRRMHD Simulations of Tidal Disruption Event Accretion Disks around Supermassive Black Holes: Jet Formation, Spectra, and Detectability