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CI Tau is a young (~2 Myr) T Tauri system with a substantial near-infraredexcess in its SED, indicating that the protoplanetary disk extends very closeto its star. This is seemingly at odds with the radial-velocity discovery of CITau b, a ~12 MJ planet at ~0.1 au, which would be expected to carve a wide,deep cavity in the innermost disk. To investigate this apparent contradiction,we run 2D hydrodynamics simulations to study the effect of the planet on thedisk, then post-process the results with radiative transfer to obtain an SED.We find that at ~0.1 au, even such a massive companion has little impact on thenear-infrared excess, a result that holds regardless of planetary eccentricityand dust size distribution. Conversely, the observed full-disk signature in CITau's SED is consistent with the existence of the hot super-Jupiter CI Tau b.As our simulations uncover, clear transition-disk signatures in SEDs are morelikely to be signposts of nascent "warm" Jupiters, located at around 1 AU inthe future habitable zones of their host stars.

CI Tau: A controlled experiment in disk-planet interaction