Table 1
List of the different astrophysical configurations that could lead to an elliptical instability (E.I) in a planetary fluid layer (liquid core, subsurface ocean) of a non synchronized or a synchronized celestial body.
| State | Origin | Origin | △ Ω | E.I | |
| of △ Ω | of β | ||||
|
|
|||||
| Non-sync. | spin rotation | D.T.a | Ωspin − Ωorb | TDEI | |
| Non-sync. | impact | S.B.a | spin-up process | TDEI | |
| Sync. | forced O.Lb | D.T. | 2eΩcos(2πt/Torb) | LDEI | |
| Sync. | forced P.Lb | S.B. | ϵΩcos(2πt/Torb) | LDEI | |
| Sync. | free P.L | S.B. | ϵΩcos(ωfreet) | LDEI | |
| Sync. | any P.L | S.B., D.T. | zonal flowc | TDEI | |
Notes. β is the ellipticity of the boundaries distortion, △ Ω is the differential rotation rate between the fluid and the elliptical deformation, Ω is the mean spin rate of the planet, ϵ is the physical libration amplitude, Torb and e are the orbital period and eccentricity, and ωfree is the free libration frequency.
Case equivalent to a non-synchronized case (cf. Sect. 2.2.2).
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