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arXiv · 0902.4328

The Dynamical Architecture and Habitable Zones of the Quintuplet Planetary System 55 Cancri

Ji Jianghui·H. Kinoshita·Liu Lin·Li Guangyu
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Abstract

We perform numerical simulations to study the secular orbital evolution and dynamical structure in the quintuplet planetary system 55 Cancri with the self-consistent orbital solutions by Fischer and coworkers (2008). In the simulations, we show that this system can be stable at least for $10^{8}$ yr. In addition, we extensively investigate the planetary configuration of four outer companions with one terrestrial planet in the wide region of 0.790 AU $\leq a \leq $ 5.900 AU to examine the existence of potential asteroid structure and Habitable Zones (HZs). We show that there are unstable regions for the orbits about 4:1, 3:1 and 5:2 mean motion resonances (MMRs) with the outermost planet in the system, and several stable orbits can remain at 3:2 and 1:1 MMRs, which is resemblance to the asteroidal belt in solar system. In a dynamical point, the proper candidate HZs for the existence of more potential terrestrial planets reside in the wide area between 1.0 AU and 2.3 AU for relatively low eccentricities.

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Ji Jianghui, H. Kinoshita, Liu Lin, Li Guangyu. 2009-02-25. The Dynamical Architecture and Habitable Zones of the Quintuplet Planetary System 55 Cancri. https://doi.org/10.1088/1674-4527/9/6/009

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