Multi-planet extrasolar systems-detection and dynamics

作     者：Cristian Beaug Sylvio Ferraz-Mello Tatiana A.Michtchenko 

作者机构：Instituto de Astronomía Teóricay ExperimentalObservatório Astronómico de CórdobaUniversidad de CórdobaArgentina Instituto de AstronomiaGeofísica e Cie ncias AtmosfricasUniversidade de So PauloBrasil 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2012年第12卷第8期

页      面：1044-1080页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：the support of CAPES  CNPq  CONICET  FAPESP and Secyt/UNC 

主　　题：planetary systems    planetary systems: formation 

摘      要：20 years after the discovery of the first planets outside our solar system, the current exoplanetary population includes more than 700 confirmed planets around main sequence stars. Approximately 50% belong to multiple-planet systems in very diverse dynamical configurations, from two-planet hierarchical systems to multiple resonances that could only have been attained as the consequence of a smooth large- scale orbital migration. The first part of this paper reviews the main detection tech- niques employed for the detection and orbital characterization of multiple-planet sys- tems, from the （now） classical radial velocity （RV） method to the use of transit time variations （TTV） for the identification of additional planetary bodies orbiting the same star. In the second part we discuss the dynamical evolution of multi-planet systems due to their mutual gravitational interactions. We analyze possible modes of motion for hi- erarchical, secular or resonant configurations, and what stability criteria can be defined in each case. In some cases, the dynamics can be well approximated by simple ana- lytical expressions for the Hamiltonian function, while other configurations can only be studied with semi-analytical or numerical tools. In particular, we show how mean- motion resonances can generate complex structures in the phase space where different libration islands and circulation domains are separated by chaotic layers. In all cases we use real exoplanetary systems as working examples.