  Of the over 800 exoplanets detected to date, over half are on non-circular
orbits, with eccentricities as high as 0.93. Such orbits lead to time-variable
stellar heating, which has implications for the planet's atmospheric dynamical
regime. However, little is known about this dynamical regime, and how it may
influence observations. Therefore, we present a systematic study of hot
Jupiters on highly eccentric orbits using the SPARC/MITgcm, a model which
couples a three-dimensional general circulation model with a plane-parallel,
two-stream, non-grey radiative transfer model. In our study, we vary the
eccentricity and orbit-average stellar flux over a wide range. We demonstrate
that the eccentric hot Jupiter regime is qualitatively similar to that of
planets on circular orbits; the planets possess a superrotating equatorial jet
and exhibit large day-night temperature variations. We show that these
day-night heating variations induce momentum fluxes equatorward to maintain the
superrotating jet throughout its orbit. As the eccentricity and/or stellar flux
is increased, the superrotating jet strengthens and narrows, due to a smaller
Rossby deformation radius. For a select number of model integrations, we
generate full-orbit lightcurves and find that the timing of transit and
secondary eclipse viewed from Earth with respect to periapse and apoapse can
greatly affect what we see in infrared (IR) lightcurves; the peak in IR flux
can lead or lag secondary eclipse depending on the geometry. For those planets
that have large day-night temperature variations and rapid rotation rates, we
find that the lightcurves exhibit "ringing" as the planet's hottest region
rotates in and out of view from Earth. These results can be used to explain
future observations of eccentric transiting exoplanets.
