2015MNRAS.448L..67D

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 (α ∼ 10^–2) around a sufficiently eccentric planet (e ∼ 0.1-0.2) and if the circumplanetary disc accretes material from its parent disc at a rate \skew4{dot}M \gtrsim 10^-7 M_☉/yr. 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.