BARNES, Rory,; DEITRICK, Russell,; GREENBERG, Richard,; QUINN, Thomas R.,; RAYMOND, Sean N.

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BARNES, Rory,
Johns Hopkins University Applied Physics Laboratory [Laurel, MD] [APL]

DEITRICK, Russell,

GREENBERG, Richard,

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Communication dans un congrès

Ce document a été publié dans

2014-11-09, Tucson. 2014-11, vol. 46, p. #210.19

Résumé en anglais

The orbital evolution of exoplanets in mean motion resonance and with mutual inclinations is often chaotic, with large amplitude variations of eccentricity 0 up to 0.9) and inclination 0 up to 170 degrees). Despite this strongly chaotic behavior, these systems can be stable for 10 Gyr. In cases that survive for only 0.1 to 1 Gyr, eccentricities can aperiodically reach values larger than 0.999 and inclinations larger than 179.9 degrees. Typically, the orbitalbehavior appears to switch between different modes, with the classic eccentricity-type resonance as one mode. Outside of that resonance, the motion cannot be easily characterized as eccentricity- and/or inclination-type, because both operate, with the conjunction longitude librating about specific directions. This phenomenon can affect Earth-mass planets in the habitable zone, potentially altering surface habitability. Planets with eccentricities that approach unity may be tidally circularized while the inclination is at any value, revealing a previously unknown process to produce misalignment between stellarspin axes and hot planets' orbital planes. Finally, we re-examine planet-planet scattering simulations and find they produce these types of systems with a frequency of order 0.5%. Giant planets exhibiting such behavior may be detectable by the GAIA spacecraft.< Réduire

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804