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Oscillations around tidal pseudo-synchronous solutions for circumbinary planets

Published online by Cambridge University Press:  30 May 2022

F. A. Zoppetti Open the ORCID record for F. A. Zoppetti [Opens in a new window] ,
H. Folonier ,
A. M. Leiva  and
C. Beaugé
F. A. Zoppetti
Affiliation:
Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba, Laprida 854, Córdoba X5000BGR, Argentina email: [email protected] CONICET, Instituto de Astronoma Teórica y Experimental, Laprida 854, Córdoba X5000BGR, Argentina
H. Folonier
Affiliation:
Instituto de Astronomia Geofsica e Ciências Atmosféricas, Universidade de São Paulo, 05508-090, Brazil
A. M. Leiva
Affiliation:
Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba, Laprida 854, Córdoba X5000BGR, Argentina email: [email protected]
C. Beaugé
Affiliation:
Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba, Laprida 854, Córdoba X5000BGR, Argentina email: [email protected] CONICET, Instituto de Astronoma Teórica y Experimental, Laprida 854, Córdoba X5000BGR, Argentina
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Abstract

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Tidal evolution of low-eccentric circumbinary planets is expected to drive the rotational evolution toward a pseudo-synchronous solution. In this work, we present a study of the oscillation amplitudes around this state by considering that the two central stars exert creep tides on the planet. These amplitudes are computed by direct numerical integrations of the creep equations and also by means of the calculation of the coefficients of the periodic terms in this stationary solution. As in the two-body-problem, the planetary spin and lag-angle are observed to have maximum oscillation amplitudes for stiff bodies and almost null oscillation for the gaseous regime, while the opposite behaviour is observed in the equatorial and polar flattenings. Our analytical approximation shows to be very accurate and specially necessary for very-low eccentric planets. However, the magnitudes of the oscillation amplitudes around the pseudo-synchronous solution in the circumbinary problem appears to be very small respect to the mean value. Thus, considering these oscillation in the computation of the tidal energy dissipation may not have a substantial contribution in the results, at least compared to the case in which only the mean values are taken into account.

Keywords

planet-star interactionsmethods: analytical
Type
Research Article
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S364: Multi-scale (Time and Mass) Dynamics of Space Objects (Oct 2021) , October 2019 , pp. 252 - 258
Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

References

Ferraz-Mello, S. 2013, Celestial Mechanics and Dynamical Astronomy, 116, 109.CrossRefGoogle Scholar
Ferraz-Mello, S. 2015, A&A, 579, A97.Google Scholar
Folonier, H. A., Ferraz-Mello, S., & Andrade-Ines, E. 2018, Celestial Mechanics and Dynamical Astronomy, 130, 78.CrossRefGoogle Scholar
Holman, M. J. & Wiegert, P. A. 1999, AJ, 117, 621.CrossRefGoogle Scholar
Mignard, F. 1979, Moon and Planets, 20, 301.CrossRefGoogle Scholar
Mills, S. M. & Mazeh, T. 2017, ApJL, 839, L8.CrossRefGoogle Scholar
Orosz, J. A., Welsh, W. F., Carter, J. A., et al. 2012, ApJ, 758, 87.CrossRefGoogle Scholar
Zoppetti, F. A., Beaugé, C., Leiva, A. M., et al. 2019, A&A, 627, A109.Google Scholar
Zoppetti, F. A., Leiva, A. M., & Beaugé, C. 2020, A&A, 634, A12.Google Scholar
Zoppetti, F. A., Folonier, H., Leiva, A. M., et al. 2021, A&A, 651, A49.Google Scholar