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Formation and evolution of planetary systems in presence of highly inclined stellar perturbers

Batygin, K. and Morbidelli, A. and Tsiganis, K. (2011) Formation and evolution of planetary systems in presence of highly inclined stellar perturbers. Astronomy and Astrophysics, 533 . Art. No. A7. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20111021-085920875

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Abstract

Context. The presence of highly eccentric extrasolar planets in binary stellar systems suggests that the Kozai effect has played an important role in shaping their dynamical architectures. However, the formation of planets in inclined binary systems poses a considerable theoretical challenge, as orbital excitation due to the Kozai resonance implies destructive, high-velocity collisions among planetesimals. Aims. To resolve the apparent difficulties posed by Kozai resonance, we seek to identify the primary physical processes responsible for inhibiting the action of Kozai cycles in protoplanetary disks. Subsequently, we seek to understand how newly-formed planetary systems transition to their observed, Kozai-dominated dynamical states. Methods. The main focus of this study is on understanding the important mechanisms at play. Thus, we rely primarily on analytical perturbation theory in our calculations. Where the analytical approach fails to suffice, we perform numerical N-body experiments. Results. We find that theoretical difficulties in planet formation arising from the presence of a distant (ã ~ 1000 AU) companion star, posed by the Kozai effect and other secular perturbations, can be overcome by a proper account of gravitational interactions within the protoplanetary disk. In particular, fast apsidal recession induced by disk self-gravity tends to erase the Kozai effect, and ensure that the disk’s unwarped, rigid structure is maintained. Subsequently, once a planetary system has formed, the Kozai effect can continue to be wiped out as a result of apsidal precession, arising from planet-planet interactions. However, if such a system undergoes a dynamical instability, its architecture may change in such a way that the Kozai effect becomes operative. Conclusions. The results presented here suggest that planetary formation in highly inclined binary systems is not stalled by perturbations, arising from the stellar companion. Consequently, planet formation in binary stars is probably no different from that around single stars on a qualitative level. Furthermore, it is likely that systems where the Kozai effect operates, underwent a transient phase of dynamical instability in the past.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201117193DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201117193&Itemid=129PublisherArticle
https://arxiv.org/abs/1106.4051arXivDiscussion Paper
Additional Information:© 2011 ESO. Received 4 May 2011; Accepted 20 June 2011. Published online 12 August 2011. We thank the referee, Y. Wu for useful suggestions.
Subject Keywords:planets and satellites: formation; planets and satellites: dynamical evolution and stability; methods: analytical; methods: numerical
Record Number:CaltechAUTHORS:20111021-085920875
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20111021-085920875
Official Citation:Formation and evolution of planetary systems in presence of highly inclined stellar perturbers K. Batygin, A. Morbidelli and K. Tsiganis A&A 533 A7 (2011) DOI: 10.1051/0004-6361/201117193
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:27346
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:21 Oct 2011 20:15
Last Modified:03 Oct 2019 03:22

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