Dynamical analysis and constraints for the HD 196885 system

Giuppone, C. A.; Morais, M. H. M.; Boué, G.; Correia, A. C. M.

doi:10.1051/0004-6361/201118356

Cited by 19 publications

(19 citation statements)

References 37 publications

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“…Therefore, we performed one simulation where the eccentricity is damped, but the semi-major axis is held constant. In this unrealistic situation, one observe that the planet migrates into the equilibrium like in Giuppone et al (2012). As a consequence, it seems that there is no inconsistency between the two models, but it becomes clear that the semi-major axis evolution plays an important role in destabilizing the Lidov-Kozai equilibria.…”

Section: Effect Of the Argument Of Periastronmentioning

confidence: 99%

“…As a consequence, it seems that there is no inconsistency between the two models, but it becomes clear that the semi-major axis evolution plays an important role in destabilizing the Lidov-Kozai equilibria. It appears that it cannot be neglected in future studies on the migration of the initial orbits as in Giuppone et al (2012).…”

Section: Effect Of the Argument Of Periastronmentioning

confidence: 99%

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Tidal damping of the mutual inclination in hierarchical systems

Correia¹,

Boué²,

Laskar³

et al. 2013

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Hierarchical two-planet systems, in which the inner body's semi-major axis is between 0.1 and 0.5 AU, usually present high eccentricity values, at least for one of the orbits. As a result of the formation process, one may expect that planetary systems with high eccentricities also have high mutual inclinations. However, here we show that tidal effects combined with gravitational interactions damp the initial mutual inclination to modest values in timescales that are shorter than the age of the system. This effect is not a direct consequence of tides on the orbits, but it results from a secular forcing of the inner planet's flattening. We then conclude that these hierarchical planetary systems are unlikely to present very high mutual inclinations, at least as long as the orbits remain outside the Lidov-Kozai libration areas. The present study can also be extended to systems of binary stars and to planet-satellite systems.

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Section: Effect Of the Argument Of Periastronmentioning

confidence: 99%

Section: Effect Of the Argument Of Periastronmentioning

confidence: 99%

Tidal damping of the mutual inclination in hierarchical systems

Correia¹,

Boué²,

Laskar³

et al. 2013

A&A

Self Cite

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“…Abrupt changes in ∆e are often traces for the presence of resonances, while regions with large variations in ∆e are more sensitive to perturbations, thus are very likely chaotic (e.g. Giuppone et al 2012;Martí et al 2013).…”

Section: Methodsmentioning

confidence: 99%

“…Indeed, in the restricted quadrupolar problem, the Hamiltonian only depends on the product e 2 cos 2ω (e.g. Kozai 1962;Giuppone et al 2012), so the initial value of ω does not change the energy at the quadrupole order, which is the dominating term. We also observe that retrograde coplanar orbits are stable for larger values of semimajor axis than prograde coplanar orbits (as also noted by Holman & Wiegert 1999;Quarles & Lissauer 2016).…”

Section: Semimajor Axis Versus Mutual Inclinationmentioning

confidence: 99%

Lidov-Kozai stability regions in the α Centauri system

Giuppone

Correia

2017

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The stability of planets in the α Centauri AB stellar system has been studied extensively. However, most studies either focus on the orbital plane of the binary or consider inclined circular orbits. Here, we numerically investigate the stability of a possible planet in the α Centauri AB binary system for S-type orbits in an arbitrary spatial configuration. In particular, we focus on inclined orbits and explore the stability for different eccentricities and orientation angles. We show that large stable and regular regions are present for very eccentric and inclined orbits, corresponding to libration in the Lidov-Kozai resonance. We additionally show that these extreme orbits can survive over the age of the system, despite the effect of tides. Our results remain qualitatively the same for any compact binary system.

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“…As a consequence, the mutual inclination, i, and the argument of the pericentre of the inner orbit measured from the line of nodes of the two orbits, ω, are also undetermined. These two parameters are critical to understanding the full dynamics of the system, but we can still place some constraints on their values (Giuppone et al 2012):…”

Section: Dynamical Evolutionmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Santerne¹,

Hébrard²,

Deleuil³

et al. 2014

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In this paper we report a new transiting warm giant planet: KOI-1257 b. It was first detected in photometry as a planet-candidate by the Kepler space telescope and then validated thanks to a radial velocity follow-up with the SOPHIE spectrograph. It orbits its host star with a period of 86.647661 d ± 3 s and a high eccentricity of 0.772 ± 0.045. The planet transits the main star of a metal-rich, relatively old binary system with stars of mass of 0.99 ± 0.05 M and 0.70 ± 0.07 M for the primary and secondary, respectively. This binary system is constrained thanks to a self-consistent modelling of the Kepler transit light curve, the SOPHIE radial velocities, line bisector and full-width half maximum (FWHM) variations, and the spectral energy distribution. However, future observations are needed to confirm it. The PASTIS fully-Bayesian software was used to validate the nature of the planet and to determine which star of the binary system is the transit host. By accounting for the dilution from the binary both in photometry and in radial velocity, we find that the planet has a mass of 1.45 ± 0.35 M , and a radius of 0.94 ± 0.12 R , and thus a bulk density of 2.1 ± 1.2 g cm −3 . The planet has an equilibrium temperature of 511 ± 50 K, making it one of the few known members of the warm-Jupiter population. The HARPS-N spectrograph was also used to observe a transit of KOI-1257 b, simultaneously with a joint amateur and professional photometric follow-up, with the aim of constraining the orbital obliquity of the planet. However, the Rossiter-McLaughlin effect was not clearly detected, resulting in poor constraints on the orbital obliquity of the planet.

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Dynamical analysis and constraints for the HD 196885 system

Cited by 19 publications

References 37 publications

Tidal damping of the mutual inclination in hierarchical systems

Tidal damping of the mutual inclination in hierarchical systems

Lidov-Kozai stability regions in the α Centauri system

SOPHIE velocimetry ofKeplertransit candidates

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