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We use the general relativistic radiation magnetohydrodynamics code\verb=KORAL= to simulate the early stages of accretion disk formation resultingfrom the tidal disruption of a solar mass star around a super massive blackhole (BH) of mass $10^6\,M_\odot$. We simulate the disruption of artificiallymore bound stars with orbital eccentricity $e\leq0.99$ (compared to the morerealistic case of parabolic orbits with $e=1$) on close orbits with impactparameter $\beta\geq3$. We use a novel method of injecting the tidal streaminto the domain. For two simulations, we choose $e=0.99$ and inject mass at arate that is similar to realistic TDEs. We find that the disk only becomesmildly circularized with eccentricity $e\approx0.6$ within the $3.5$ days thatwe simulate. The rate of circularization is faster for pericenter radii thatcome closer to the BH. The emitted radiation is mildly super-Eddington with$L_{\rm{bol}}\approx3-5\,L_{\rm{Edd}}$ and the photosphere is highly asymmetricwith the photosphere being significantly closer to the inner accretion disk forviewing angles near pericenter. We find that soft X-ray radiation with$T_{\rm{rad}} \approx 3-5\times 10^5$ K may be visible for chance viewingangles. Our simulations predict that TDEs should be radiatively inefficientwith $\eta\approx0.009-0.014$. These are the first simulations whichsimultaneously capture the stream, disk formation, and emitted radiation.

Global Simulations of Tidal Disruption Event Disk Formation via Stream Injection in GRRMHD