Commission 7: Celestial Mechanics and Dynamical Astronomy
| Autor: | C. Beaugé, David Vokrouhlický, Andrea Milani, Anne Lemaitre, Zoran Knežević, D.C. Heggie, Joseph A. Burns, Andrzej J. Maciejewski, Alessandro Morbidelli, B. Erdi, Toshio Fukushima, J.-L. Zhou, John D. Hadjidemetriou, M. Sidlichovský |
|---|---|
| Přispěvatelé: | Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2010 |
| Předmět: |
Orbital elements
Physics 010504 meteorology & atmospheric sciences Computer Science::Information Retrieval Quantum Monte Carlo 010102 general mathematics Monte Carlo method Astronomy and Astrophysics Markov chain Monte Carlo Planetary system 01 natural sciences Celestial mechanics Radial velocity symbols.namesake Classical mechanics Space and Planetary Science 0103 physical sciences Orbit (dynamics) symbols Astrophysics::Earth and Planetary Astrophysics Statistical physics 0101 mathematics 010303 astronomy & astrophysics ComputingMilieux_MISCELLANEOUS 0105 earth and related environmental sciences |
| Zdroj: | Transactions of the International Astronomical Union, Series B Transactions of the International Astronomical Union, Series B, The International Astronomical Union, 2010, 27, pp.120-122. ⟨10.1017/s1743921310004874⟩ |
| Popis: | The orbital fits of multi-planetary systems from radial velocity data has proved to be a complex task. In some cases, different orbital solutions provide similarly good fits, especially when two planets are near mean-motion resonances. Ferraz-Melloet al(2005) and Goździewskiet al(2005) showed that the published best fits of systemsHD82932andHD160691are dynamically unstable, and re-determined their orbital parameters with Monte Carlo and genetic algorithms. In both cases dynamically stable orbits were found with RMS similar to the published orbits. It was also shown that uncertainties in the stellar mass Ferraz Melloet al(2005) and the stellar jitter Gozdziewskiet al(2005) can significantly affect the orbital determination. Ford (2005) used a Markov chain Monte Carlo technique to quantify the orbit uncertainties. For some planetary systems he found a strong correlation between the orbital elements and/or significant non-Gaussian error distribution in the parameter space. As a consequence, the actual uncertainties in the orbital fits can be much larger (or smaller) than those published. |
| Databáze: | OpenAIRE |
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