of $(\frac{1+e}{1-e})^2$). For example, if $e = 0.3$, the stellar flux varies by $\sim$3.5 along its orbit. For $e$ = 0.6, this variation is a factor of 16! Such eccentricities are by no means rare in the sample of known EGPs (cf. Table 1). Therefore, it is possible for the composition of an EGP atmosphere to change significantly during its orbit, for clouds to appear and disappear, and for there to be delays (“hysteresis") in the accommodation of a planet’s atmosphere to a varying “insolation" regime. Ignoring the latter, eqs. \[falpha\] and \[cosinef\] can be combined with $\Phi(\alpha)$ and the standard Keplerian formula connecting $\theta$ and time for an orbit with a given $P$ and $e$ to derive an EGP’s light curve as a function of wavelength, $i$, $e$, $\Omega$, $\omega$, and time. The upshot is that, depending upon orientation and eccentricity, the brightness of an EGP can vary in its orbit not at all (for a face-on EGP in a circular orbit) or quite dramatically (e.g., for highly eccentric orbits at high inclination angles). Since astrometric measurements of stellar wobble induced by EGPs can yield the entire orbit (including inclination), data from the Space Interferometry Mission (SIM)[@UnwinShao00] (expected to 