Cezary Migaszewski, Mariusz Slonina, Krzysztof Gozdziewski
The Kepler-11 star hosts at least six transiting super-Earth planets detected through the precision photometric observations of the KEPLER mission (Lissauer et al.). In this paper, we re-analyze the available KEPLER data, using the direct N-body approach rather than an indirect TTV method in the discovery paper. The orbital modeling in the realm of the direct approach relies on the whole data set, rather than the times of mid-transits only. Most of the results in the original paper are confirmed and extended. We constrained the mass of the outermost planet g to less than 30 Earth masses. The mutual inclinations between orbits b and c as well as between orbits d and e are determined with a good precision, in the range of [1,5] degrees. Having several solutions to four qualitative orbital models of the Kepler-11 system, we analyze its global dynamics with the help of dynamical maps. They reveal very complex structure of the phase space with narrow regions of regular motion. The dynamics are governed by a dense net of three- and four-body mean motion resonances, forming the Arnold web. Overlapping of these resonances is a main source of instability. We found that the Kepler-11 system may be long-term stable only in particular multiple resonant configurations with small relative inclinations. The mass-radius data derived for all companions reveal a clear anti-correlation between the mean density of the planets with their distance from the star. It may reflect the formation and early evolution history of the system.
View original:
http://arxiv.org/abs/1205.0822
No comments:
Post a Comment