Dynamical Evolution of Planetary Systems View Full Text


Ontology type: schema:Chapter      Open Access: True


Chapter Info

DATE

2018-11-03

AUTHORS

Alessandro Morbidelli

ABSTRACT

Planetary systems can evolve dynamically even after the full growth of the planets themselves. There is actually circumstantial evidence that most planetary systems become unstable after the disappearance of gas from the protoplanetary disk. These instabilities can be due to the original system being too crowded and too closely packed or to external perturbations such as tides, planetesimal scattering, or torques from distant stellar companions. The Solar System was not exceptional in this sense. In its inner part, a crowded system of planetary embryos became unstable, leading to a series of mutual impacts that built the terrestrial planets on a timescale of ∼100 My. In its outer part, the giant planets became temporarily unstable, and their orbital configuration expanded under the effect of mutual encounters. A planet might have been ejected in this phase. Thus, the orbital distributions of planetary systems that we observe today, both solar and extrasolar ones, can be different from those emerging from the formation process, and it is important to consider possible long-term evolutionary effects to connect the two. More... »

PAGES

2523-2541

Book

TITLE

Handbook of Exoplanets

ISBN

978-3-319-55332-0
978-3-319-55333-7

Author Affiliations

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-3-319-55333-7_145

DOI

http://dx.doi.org/10.1007/978-3-319-55333-7_145

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1107988008


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