  We use the general relativistic radiation magnetohydrodynamics code
\verb=KORAL= to simulate the early stages of accretion disk formation resulting
from the tidal disruption of a solar mass star around a super massive black
hole (BH) of mass $10^6\,M_\odot$. We simulate the disruption of artificially
more bound stars with orbital eccentricity $e\leq0.99$ (compared to the more
realistic case of parabolic orbits with $e=1$) on close orbits with impact
parameter $\beta\geq3$. We use a novel method of injecting the tidal stream
into the domain. For two simulations, we choose $e=0.99$ and inject mass at a
rate that is similar to realistic TDEs. We find that the disk only becomes
mildly circularized with eccentricity $e\approx0.6$ within the $3.5$ days that
we simulate. The rate of circularization is faster for pericenter radii that
come 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 asymmetric
with the photosphere being significantly closer to the inner accretion disk for
viewing 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 viewing
angles. Our simulations predict that TDEs should be radiatively inefficient
with $\eta\approx0.009-0.014$. These are the first simulations which
simultaneously capture the stream, disk formation, and emitted radiation.
