Theory of motion of saturn's coorbiting satellites

Yoder, C. F.; Colombo, G.; Synnott, S. P.; Yoder, K.A.

doi:10.1016/0019-1035(83)90207-5

Cited by 115 publications

(91 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our prediction for the effects of Jupiter's radial migration, however, disagrees with Yoder's 1979 result (see Table I). Statements in Yoder et al (1983) about the tidal evolution of the Saturnian satellites Janus and Epimetheus, however, are inconsistent with Yoder's 1979 calculations, but agree, at least in sign, with our radial migration results. In order to dispel this confusion, we carefully verify our analytic predictions with numerical simulations in sections 3 and 4 below.…”

Section: Insert Figurecontrasting

confidence: 64%

On the Origin of the Trojan Asteroids: Effects of Jupiter's Mass Accretion and Radial Migration

Fleming

Hamilton

2000

Icarus

View full text Add to dashboard Cite

Section: Insert Figurecontrasting

confidence: 64%

On the Origin of the Trojan Asteroids: Effects of Jupiter's Mass Accretion and Radial Migration

Fleming

Hamilton

2000

Icarus

View full text Add to dashboard Cite

“…In the rotating frame, they have synchronized horseshoe-like libration motions that prevent them from colliding. The less massive one has the largest amplitude motion (Yoder et al 1983). The associated libration period is here again a few hundred orbital periods of the primaries.…”

Section: Planet(s) Around θ Cygnimentioning

confidence: 99%

Extrasolar planets and brown dwarfs around A–F type stars

Desort¹,

Lagrange²,

Galland³

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. In the framework of the search for extrasolar planets and brown dwarfs around early-type main-sequence stars, we present the results obtained on the early F-type star θ Cygni. Methods. ELODIE and SOPHIE at the Observatoire de Haute-Provence (OHP) were used to obtain 91 and 162 spectra, respectively. Our dedicated radial-velocity measurement method was used to monitor the star's radial velocities over five years. We also used complementary, high angular resolution and high-contrast images taken with PUEO at the CFHT. Results. We show that θ Cygni radial velocities are quasi-periodically variable, with a 150-day period. These variations are not due to the 0.35-M stellar companion that we detected in imaging at more than 46 AU from the star. The absence of correlation between the bisector velocity span variations and the radial velocity variations for this 7 km s −1 v sin i star, as well as other criteria, indicate that the observed radial velocity variations do not stem from stellar spots. The observed amplitude of the bisector velocity span variations also seems to rule out stellar pulsations. However, we observe a peak in the bisector velocity span periodogram at the same period as the one found in the radial velocity periodogram, which indicates a probable link between these radial velocity variations and the low-amplitude lineshape variations with a stellar origin. Long-period variations are not expected from this type of star to our knowledge. If a stellar origin (hence of new type) were to be confirmed for these long-period radial velocity variations, this would have several consequences on the search for planets around main-sequence stars, both in terms of observational strategy and data analysis. An alternative explanation for these variable radial velocities is the presence of at least one planet of a few Jupiter masses orbiting at less than 1 AU; however, this planet alone does not explain all observed features, and the θ Cygni system is obviously more complex than a planetary system with 1 or 2 planets. Conclusions. The available data do not allow us to distinguish between these two possible origins. A vigourous follow-up in spectroscopy and photometry is needed to get a comprehensive view of the star intrinsic variability and/or its surrounding planetary system. Key words. techniques: radial velocities -stars: early-type -stars: planetary systems -stars: individual: θ Cygni Based on observations made with the ELODIE and SOPHIE spectrographs at the Observatoire de Haute-Provence (CNRS, France) and with the PUEO adaptive optics system at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National

show abstract

“…For example Dermott & Murray, 1981, Spirig & Waldvogel, 1985, Waldvogel & Spirig, 1988and Auner, 2001 [1] studied the horseshoe motion by perturbation theory and numerical experiments. Yoder et al, 1983Yoder et al, , 1989 developed an analytic approximation for the Exchange-a motion. Llibre & Ollé, 2001 proved the existence of stable planar horseshoe periodic orbits for the Saturn-Janus mass parameter in the restricted circular three-body problem.…”

Section: Introductionmentioning

confidence: 99%

Exchange orbits: an interesting case of co-orbital motion

Funk¹,

Dvořák²,

Schwarz³

2013

Celest Mech Dyn Astr

View full text Add to dashboard Cite

In this investigation we treat a special configuration of two celestial bodies in 1:1 mean motion resonance namely the so-called exchange orbits. There exist -at least -theoretically -two different types: the exchange-a orbits and the exchange-e orbits. The first one is the following: two celestial bodies are in orbit around a central body with almost the same semi-major axes on circular orbits. Because of the relatively small differences in semi-major axes they meet from time to time and exchange their semi-major axes. The inner one then moves outside the other planet and vice versa. The second configuration one is the following: two planets are moving on nearly the same orbit with respect to the semi-major axes, one on a circular orbit and the other one on an eccentric one. During their dynamical evolution they change the characteristics of the orbit, the circular one becomes an elliptic one whereas the elliptic one changes its shape to a circle. This 'game' repeats periodically. In this new study we extend the numerical computations for both of these exchange orbits to the three dimensional case and in another extension treat also the problem when these orbits are perturbed from a fourth body. Our results in form of graphs show quite well that for a large variety of initial conditions both configurations are stable and stay in this exchange orbits.

show abstract

Theory of motion of saturn's coorbiting satellites

Cited by 115 publications

References 19 publications

On the Origin of the Trojan Asteroids: Effects of Jupiter's Mass Accretion and Radial Migration

On the Origin of the Trojan Asteroids: Effects of Jupiter's Mass Accretion and Radial Migration

Extrasolar planets and brown dwarfs around A–F type stars

Exchange orbits: an interesting case of co-orbital motion

Contact Info

Product

Resources

About