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The Stable Topology of the Planetary Systems of two 2:1 Resonant Companions:Application to HD 82943 | | Ji Jianghui
; H. Kinoshita
; Liu Lin
; H. Nakai
; Li Guangyu
; | | Date: |
29 Dec 2004 | | Subject: | astro-ph | | Affiliation: | 1,3), H. Kinoshita , Liu Lin (2,3), H. Nakai , Li Guangyu (1,3) (Purple Mountain Observatory, Nanjing Univ., NAOC, NAOJ | | Abstract: | We have numerically explored the stable planetary geometry for the multiple systems involved in a 2:1 mean motion resonance, and herein we mainly study the HD 82943 system by employing two sets of the orbital parameters (Mayor et al. 2004; Ji et al. 2004). In the simulations, we find that all stable orbits are related to the 2:1 resonance that can help to remain the semi-major axes for two companions almost unaltered over the secular evolution for $10^{8}$ yr. In addition, we also show that there exist three possible stable configurations:(1) Type I, only $ heta_{1} approx 0^{circ}$, (2) Type II, $ heta_{1}approx heta_{2}approx heta_{3}approx 0^{circ}$ (aligned case), and (3) Type III, $ heta_{1}approx 180^{circ}$, $ heta_{2}approx0^{circ}$, $ heta_{3}approx180^{circ}$ (antialigned case), where two resonant arguments are $ heta_{1} = lambda_{1} - 2lambda _{2} + varpi_{1}$ and $ heta_{2} = lambda_{1} - 2lambda_{2} + varpi_{2}$, the relative apsidal longitudes $ heta_{3} = varpi_{1}-varpi_{2}=Deltavarpi$. And we find that other 2:1 resonant systems (e.g., GJ 876) may possess one of three stable orbits in their realistic motions. Moreover, we also study the existence of the assumed terrestrial bodies at $sim 1$ AU for HD 82943 and GJ 876 systems (see main texts). | | Source: | arXiv, astro-ph/0501651 | | Services: | Forum | Review | PDF | Favorites | |
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