Stability and eccentricity of periodic orbit for two planets in a 1:1 resonance
| dc.creator | Nauenberg, Michael | |
| dc.date | 2002-04-14 | |
| dc.date.accessioned | 2026-07-25T11:44:27Z | |
| dc.description | The nonlinear stability domain of Lagrange's celebrated 1772 solution of a three-body problem is obtained numerically as a function of the masses of the bodies and the common eccentricity of their Keplerian orbits. This domain shows that this solution may be realized in extra-solar planetary systems similar to those that have been discovered recently with two Jupiter-size planets orbiting a solar-size star. For an exact 1:1 resonance, the Doppler shift variation in the emitted light would be the same as for stars which have only a single planetary companion. But it is more likely that in actual extra-solar planetary systems there are deviations from such a resonance, raising the interesting prospect that Lagrange's solution can be identified by an analysis of the observations. The existence of another stable 1:1 resonance solution which would have a more unambiguous Doppler shift signature is also discussed. | |
| dc.description | 9 pages 11 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0204228 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0204228 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/5233 | |
| dc.subject | Astrophysics | |
| dc.title | Stability and eccentricity of periodic orbit for two planets in a 1:1 resonance | |
| dc.type | text |