We investigate the origins of Kepler-419, a peculiar system hosting two nearly coplanar and highly eccentric gas giants with apsidal orientations liberating around anti-alignment, and use this system to place constraints on the properties of their birth protoplanetary disk. We follow the proposal by Petrovich, Wu, & Ali-Dib (2019) that these planets have been naturally placed on these orbits as a result of the precessional effects of a slowly dissipating massive disk and extend it by using direct N-body simulations and models for the evolution of the gas disks, including photo-evaporation. Based on a parameter space exploration, we find that in order to reproduce the system the initial disk mass had to be at least 95 MJup and dissipate on a timescale of at least 104 yr. This mass is consistent with the upper end of the disks mass observed distribution, and the dissipation timescale is consistent with photoevaporation models. We study the properties of such disks using simplified 1D thin disk models and show that they are gravitationally stable, indicating that the two planets must have formed via core accretion and thus prone to disk migration. We hence finally investigate the sensitivity of this mechanism to the outer planet’s semi major axis, and find that the nearby 7:1, 8:1, and 9:1 mean-motion resonances can completely quench this mechanism, while even higher order resonances can also significantly affect the system. Assuming the two planets avoid these high order resonances and/or close encounters, the dynamics seems to be rather insensitive to planet c semi major axis, and thus disk migration.
Ali-Dib & Petrovich (2020) MNRAS.