The Stable Topology of the Planetary Systems of two 2:1 Resonant Companions:Application to HD 82943

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dc.creatorJianghui, Ji
dc.creatorKinoshita, H.
dc.creatorLin, Liu
dc.creatorNakai, H.
dc.creatorGuangyu, Li
dc.date2005-01-29
dc.date.accessioned2026-07-07T02:16:53Z
dc.date.available2026-07-07T02:16:53Z
dc.descriptionWe 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 $θ_{1} \approx 0^{\circ}$, (2) Type II, $θ_{1}\approxθ_{2}\approxθ_{3}\approx 0^{\circ}$ (aligned case), and (3) Type III, $θ_{1}\approx 180^{\circ}$, $θ_{2}\approx0^{\circ}$, $θ_{3}\approx180^{\circ}$ (antialigned case), where two resonant arguments are $θ_{1} = λ_{1} - 2λ_{2} + \varpi_{1}$ and $θ_{2} = λ_{1} - 2λ_{2} + \varpi_{2}$, the relative apsidal longitudes $θ_{3} = \varpi_{1}-\varpi_{2}=Δ\varpi$. 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).
dc.description9 pages, 4 figures, submitted to Advances in Space Research, proceeding of COSPAR 2004, Paris
dc.identifierhttps://arxiv.org/abs/astro-ph/0501651
dc.identifierhttp://arxiv.org/abs/astro-ph/0501651
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8965
dc.subjectAstrophysics
dc.titleThe Stable Topology of the Planetary Systems of two 2:1 Resonant Companions:Application to HD 82943
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