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On the stability of Earth-like planets in multi-planet systems |
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| Authors: | E Pilat-Lohinger P Robutel Á Süli F Freistetter |
| Institution: | 1. Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180, Vienna, Austria 2. Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR 2028, Observatoire de Paris, 77 Av. Denfert-Rochereau, 75014, Paris, France 3. Department of Astronomy, E?tv?s University, XI. Pázmány Péter sétány 1/A, 1117, Budapest, Hungary 4. Astrophysikalisches Institut, Friedrich-Schiller-Universit?t Jena, Schillerg?sschen 2-3, 07745, Jena, Germany |
| Abstract: | We present a continuation of our numerical study on planetary systems with similar characteristics to the Solar System. This time we examine the influence of three giant planets on the motion of terrestrial-like planets in the habitable zone (HZ). Using the Jupiter–Saturn–Uranus configuration we create similar fictitious systems by varying Saturn’s semi-major axis from 8 to 11 AU and increasing its mass by factors of 2–30. The analysis of the different systems shows the following interesting results: (i) Using the masses of the Solar System for the three giant planets, our study indicates a maximum eccentricity (max-e) of nearly 0.3 for a test-planet placed at the position of Venus. Such a high eccentricity was already found in our previous study of Jupiter–Saturn systems. Perturbations associated with the secular frequency g 5 are again responsible for this high eccentricity. (ii) An increase of the Saturn-mass causes stronger perturbations around the position of the Earth and in the outer HZ. The latter is certainly due to gravitational interaction between Saturn and Uranus. (iii) The Saturn-mass increased by a factor 5 or higher indicates high eccentricities for a test-planet placed at the position of Mars. So that a crossing of the Earth’ orbit might occur in some cases. Furthermore, we present the maximum eccentricity of a test-planet placed in the Earth’ orbit for all positions (from 8 to 11 AU) and masses (increased up to a factor of 30) of Saturn. It can be seen that already a double-mass Saturn moving in its actual orbit causes an increase of the eccentricity up to 0.2 of a test-planet placed at Earth’s position. A more massive Saturn orbiting the Sun outside the 5:2 mean motion resonance (a S ≥9.7 AU) increases the eccentricity of a test-planet up to 0.4. |
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