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Title:
Tidal dissipation in multi-planet systems and constraints on orbit fitting
Authors:
Laskar, J.; Boué, G.; Correia, A. C. M.
Affiliation:
AA(Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014, Paris, France ), AB(Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014, Paris, France; Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal), AC(Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014, Paris, France; Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193, Aveiro, Portugal)
Publication:
Astronomy & Astrophysics, Volume 538, id.A105, 7 pp. (A&A Homepage)
Publication Date:
02/2012
Origin:
EDP Sciences
Astronomy Keywords:
methods: analytical, celestial mechanics, planets and satellites: general
DOI:
10.1051/0004-6361/201116643
Bibliographic Code:
2012A&A...538A.105L

Abstract

We present here in full detail the linear secular theory with tidal damping that was used to constrain the fit to the HD 10180 planetary system in Lovis et al. (2011, A&A, 528, A112). The theory is very general and can provide some intuitive understanding of the final state of a planetary system when one or more planets are close to their central star. We globally recover the results of Mardling (2007, MNRAS, 382, 1768). However, for the HD 209458 planetary system, we show that the consideration of the tides raised by the central star on the planet leads one to believe that the eccentricity of HD 209458b is most probably much smaller than 0.01.
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