- Alessandro Morbidelli (OCA- President C7)
- Alain Levavalier des Etains (IAP-President C53)
- Jacques Laskar (IMCCE-Vice Pres. Div.A)
- Nader Haghighipour (IFA-Vice Pres. Div. F)
Scientific Organizing Committee
- J.L. Zhou (NJU)
- S. Ida (ELSI)
- T.A. Mictchenko (USP)
- E. Ford (UFL)
- C. Terquem (University of Oxford)
- R. Mardling (Monash University, Geneva Observatory)
- Dynamical evolution of planetary systems,
- Origin of "hot" planets, origin of large eccentricities and orbital obliquities,
- tidal and resonant effects
- FM1.2.03 Antoine Strugarek: Close-in Planet Migration due to Magnetic Torques
- FM1.4.02 Tiago Campante: Spin-orbit Alignment of Exoplanet Systems: How Can Asteroseismology Help Us?
The number of known extrasolar planets has increased considerably over the last years. Today, we have cataloged about 1000 confirmed planets (plus over 3000 planet candidates of the Kepler mission), a good fraction of which are in more than 130 multi-planet systems. The discovery of these systems has raised many interesting questions on their formation and dynamical evolution.
Planets in mean motion resonances prompt the investigation of resonant dynamics in the framework of the general (i.e. non-restricted) three-body problem. The general problem is much more complicated than the restricted one, so that we have yet to achieve a global description of resonant dynamics. While previous observations have identified several multi-planet systems in mean-motion resonances, recent observations point to systems of small planets which seem to lie close to resonances, but outside the libration domains. The reason for these near-resonance configurations is not yet clear: tidal evolution could have played a role in extracting planets from resonance, and so might turbulence in the original proto-planetary disk.
The origin of "hot" planets (planets with orbital periods of a few days) is still a matter of debate: did these planets reach their orbit by migrating through the proto-planetary disk, or did they arrive at their current orbital configurations via scattering and tidal damping?
The origin of the surprisingly large eccentricities and/or inclinations (relative to the stellar equator) of many extrasolar planets remains elusive: planet instabilities, planet-disk interactions, external perturbations from eccentric or inclined stars remain viable options.
This (non-exhaustive) list of open problems highlights the importance of dynamical studies for understanding the nature of the systems that are observed, as well as establishing clues on their origin.
Moreover, it is important to stress that dynamical models can also complement observations for a better characterization of extrasolar planets. Dynamical maps have been very useful to constrain the orbits of multi-planet systems, for which the uncertainties in the orbital parameters due to the observational errors are often much wider than the range of orbital configurations permitting the long-term stability of the system. A special mention has to be given to Transit Time Variations (TTV) analyses. TTVs are now routinely detected in packed systems of multiple planets. They are used to confirm planet candidates and they allow the determination of the masses of the planets. The power and success of this technique can be emphasized by the recent discovery and orbital determination of a non-transiting planet, through the analysis of the TTV signal of a transiting companion. The TTV method brings Celestial Mechanics back to the glorious time when Le Verrier predicted the existence and the position of Neptune from the analysis of the anomalies of the motion of Uranus.
Last but not least, dynamical studies are essential to determine whether a given planet can remain stable in the habitable zone, whether it should be tidally locked in a spin-orbit resonance etc.
All these examples show that the synergy between dynamicists and observers is a key to the advancement of extrasolar planet science. The studies of the solar system during the past several decades have proven that the understanding of our own planetary system can leap forward only with the combination of dynamical modeling and physical observations. The time has now come to extend this synergy to a larger number of planetary systems.
We believe that the organization of a focused meeting on dynamical problems in extrasolar planets during the 2015 GA will be the best way to facilitate such synergy by bringing together scientists from different communities of planetary science.