Abstract
The recent increase in number of known multi-planet systems gives a unique opportunity to study the processes responsible for planetary formation and evolution. Special attention is given to the occurrence of mean-motion resonances, because they carry important information about the history of the planetary systems. At the early stages of the evolution, when planets are still embedded in a gaseous disc, the tidal interactions between the disc and planets cause the planetary orbital migration. The convergent differential migration of two planets embedded in a gaseous disc may result in the capture into a mean-motion resonance. The orbital migration taking place during the early phases of the planetary system formation may play an important role in shaping stable planetary configurations. An understanding of this stage of the evolution will provide insight on the most frequently formed architectures, which in turn are relevant for determining the planet habitability. The aim of this paper is to present the observational properties of these planetary systems which contain confirmed or suspected resonant configurations. A complete list of known systems with such configurations is given. This list will be kept by us updated from now on and it will be a valuable reference for studying the dynamics of extrasolar systems and testing theoretical predictions concerned with the origin and the evolution of planets, which are the most plausible places for existence and development of life.
Highlights
Studies of the formation and evolution of planetary systems have entered into a new extremely dynamic phase of the development
One of the main reasons for that is the fact that the Solar System is no longer the only planetary system known in our Galaxy
After the work of Copernicus (1543), Kepler (1609, 1619), Galilei (1632) and Newton (1687), it became clear that the observed motion of the objects in our planetary system is a consequence of the gravitational force
Summary
Studies of the formation and evolution of planetary systems have entered into a new extremely dynamic phase of the development. Many other planetary systems have been discovered till and they are observed at different stages of their evolution They provide distinct realizations of the same set of processes which were responsible for the formation of our Solar System. The attempt to model the relative distances of planets in the Solar System is known today as the Titius–Bode law This empirical law in its original form states that the mean distance d from the Sun to each of the six (known to Titius) planets can be approximated by the relation d = 0.4 + 0.3 × 2i,. The mean-motion resonances may protect the planets (satellites) from close encounters and enhance the stability of the systems in the long term. It is so important to understand the process of the formation of the mean-motion resonances in the early stages of the planetary system evolution
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