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Multiple-planet Scattering and the Origin of Hot Jupiters

  • Authors: C. Beaugé and D. Nesvorný

Beaugé & Nesvorný 2012 The Astrophysical Journal 751 119.

  • Provider: AAS Journals

Caption: Figure 1.

Tidal evolution of a Jovian-mass planet with initial semimajor axis a 1 = 0.04 AU and e 1 = 0.05. P 0 is the stellar rotation period, while P 1 is the planet's rotation period. The dashed green line in the bottom-left panel shows the planet's orbital period. The stellar and planetary obliquities (θ 0 and θ 1, respectively) are shown in the bottom-right panel and measured with respect to the inner planet's orbital plane. Both spin axes where initially chosen parallel to the orbital angular momentum vector.

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