Are Eccentric Protoplanetary Disk Always Misaligned?

Planet-disk combinations, where a protoplanetary disk has an observed embedded planet, remain a rare occurrence that can provide an exciting and unique opportunity to test the theory of planet-disk interaction, which is fundamental to our understanding of planet formation. CI Tau is one such system with radial velocity observations of a 11.29 ± 2.16 [MJ] planet at 0.085 ± 0.001 au while new RV observations now predicts a period of 23.86 ± 0.04 days, orbit radius of 0.156 ± 0.002 au, and a mass of 3.70+0.80−0.66 [MJ]. Notably, recent Ro-Vibrational observations with 12CO shows a first-of-its-kind eccentric inner-outer disk anti-alignment with the break at 0.14 ± 0.08 au. We performed hydrodynamical, piecewise parabolic simulations with PEnGUIn modeling the CI Tau disk with these previous and recent parameters. The previous estimates of CI Tau b create a wide-deep gap that was not observed nor could reproduce the disk misalignment break at 0.14 ± 0.08 au. Using the recent estimates for CI Tau b, we have been able to reproduce the observed radial break and various regimes of disk misalignment while conforming to the period of 23.86 ± 0.04 days. These regimes are driven potentially by competing Eccentric Planet and Eccentric Disk Lindblad Resonance which are both exciting and dampening the disk eccentricity. With additional pipeline synthetic observation codes, we have found regimes of agreement between real and synthetic Ro-Vibrational observations. From these regimes of agreement, we now possess for the first time the ability to predict near-future disk misalignment periapsis angles for a misalignment inner-outer disk. With near-future Ro-Vibrational observations, we will be able to significantly constrain the planet-disk parameters of CI Tau; grounding our theoretical knowledge in observations.