  I present the results of 1D models of circumplanetary discs around planets on
eccentric orbits. I use a classical viscous heating model to calculate emission
fluxes at the wavelengths targeted by the NIRCam instrument on JWST, and
compare the variability of this signal with the published NIRCam sensitivity
specifications. This variability is theoretically detectable by JWST for a
sufficiently viscous disc ($\alpha \sim 10^{-2}$) around a sufficiently
eccentric planet ($e \sim 0.1-0.2$) and if the circumplanetary disc accretes
material from its parent disc at a rate $\dot{M} \gtrsim 10^{-7}\,
\mathrm{M}_{\odot}\,\mathrm{yr}^{-1}$. I discuss the limitations of the models
used, and the implications of the result for probing the effectiveness of disc
interactions for growing a planet's orbital eccentricity.
