  We present general relativistic radiation magnetohydrodynamics (GRRMHD)
simulations of super-Eddington accretion flows around supermassive black holes
(SMBHs) which may apply to tidal disruption events (TDEs). We perform long
duration ($t\geq81,200\, GM/c^3$) simulations which achieve mass accretion
rates $\gtrsim 11$ times the Eddington rate and produce thermal synchrotron
spectra and images of their jets. The jet reaches a maximum velocity of $v/c
\approx 0.5-0.9$, but the density weighted outflow velocity is $\sim0.2-0.35c$.
Gas flowing beyond the funnel wall expands conically and drives a strong shock
at the jet head while variable mass ejection along the jet axis results in
internal shocks and dissipation. For a $T_i/T_e=1$ model, the
radio/submillimeter spectra peak at $>100$ GHz and the luminosity increases
with BH spin, exceeding $\sim 10^{41} \, \rm{erg\, s^{-1}}$ in the brightest
models. The emission is extremely sensitive to $T_i/T_e$ as some models show an
order of magnitude decrease in the peak frequency and up to four orders of
magnitude decline in their radio/submillimeter luminosity as $T_i/T_e$
approaches 20. Assuming a maximum VLBI baseline distance of $10 \
{\rm{G}}\lambda$, 230 GHz images of $T_i/T_e=1$ models shows that the jet head
may be bright enough for its motion to be captured with the EHT (ngEHT) at
$D\lesssim110$ (180) Mpc at the $5\sigma$ significance level. Resolving
emission from internal shocks requires $D\lesssim45$ Mpc for both the EHT or
ngEHT. The 5 GHz emission in each model is dimmer ($\lesssim10^{36} \
{\rm{erg\, s^{-1}}}$) than upper limits placed on TDEs with no radio emission
which suggests jets similar to our models may have gone undetected in previous
observations. Our models suggest that the ngEHT may be utilized for $>230$ GHz
radio/submillimeter followup of future TDEs.
