Excitation of planetary inclinations via dynamical bifurcations driven by misaligned disks

Open Access

Fig. 1

Geometric illustration of a multi-planet system with a misaligned protoplanetary disk. The disk’s angular momentum orientation is denoted by the unit vector ${\hat{l}}_{d}$ $\[\hat{\boldsymbol{l}}_{\mathrm{d}}\]$ . The host star rotates at angular velocity Ω_⋆ with its spin oriented along ${\hat{s}}_{⋆}$ $\[\hat{\boldsymbol{s}}_{\star}\]$ . The primordial stellar obliquity (ψ_⋆0) corresponds to the angle between ${\hat{l}}_{d}$ $\[\hat{\boldsymbol{l}}_{\mathrm{d}}\]$ and ${\hat{s}}_{⋆}$ $\[\hat{\boldsymbol{s}}_{\star}\]$ . The angle between the planet’s orbit angular momentum vector (l₁) and ${\hat{s}}_{⋆}$ $\[\hat{\boldsymbol{s}}_{\star}\]$ is referred to as the stellar obliquity (ψ_1⋆).

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