  We calculate the high energy (sub-GeV to TeV) prompt and afterglow emission
of GRB 080319B that was distinguished by a naked-eye optical flash and by an
unusual strong early X-ray afterglow. There are three possible sources for high
energy emission: the prompt optical and $\gamma$-ray photons IC scattered by
the accelerated electrons, the prompt photons IC scattered by the early
external reverse-forward shock electrons, and the higher band of the
synchrotron and the synchrotron self-Compton emission of the external shock.
There should have been in total {hundreds} high energy photons detectable for
the Large Area Telescope (LAT) onboard the Fermi satellite, and {tens} photons
of those with energy $> 10$ GeV. The $> 10$ GeV emission had a duration about
twice that of the soft $\gamma$-rays. AGILE could have observed these energetic
signals if it was not occulted by the Earth at that moment. The physical
origins of the high energy emission detected in GRB 080514B, GRB 080916C and
GRB 081024B are also discussed. These observations seem to be consistent with
the current high energy emission models.
