We also discuss the possible relationship between the current orbital elements fits of known exoplanets in the 2/1 mean-motion resonance and the expected orbital configuration due to migration. We find that, as long as the orbital decay was sufficiently slow to be approximated by an adiabatic ...
Thus, chaotic diffusion of the orbital elements can be quite slow, while there can also exist a nonnegligible set of chaotic orbits which are semiconfined (stable chaos) by "quasi-barriers" in the phase space. In the present paper we extend our study to all mean motion resonances of order...
This was shown not to be due to calibrational errors but, apparently, to the need for improvement of other orbital elements-at least for Proteus. Despite this anomaly, the mean motion accuracies were improved by almost 2 orders of magnitude as a result of the longer baseline since the ...
We take typical orbital elements (e,i) for different populations and calculate the strength of all resonances verifying |p+q|<100 and order q<100 with all the planets from Mercury to Neptune. In the region between 0 and 6 AU we used typical orbital elements of Conclusions According to the...
Which of the following statements about how halo stars compare to our Sun is not true? a) Most stars in the halo are younger than our Sun. b) Most stars in the halo contain a much lower percentage of heavy elements than our Sun. c) Most stars...
In this paper we briefly study changes in the mean seasonal insolations on the planet Mars caused by significant large-scale variations in the following orbital elements: the eccentricity ( e ), the obliquity (ε) and the longitude of perihelion (λ p ). Three orbital configurations have been...
Orbital ElementsPlanetsPrecessionEccentricityEphemeridesOccultationPerihelionsWe present, in this paper, a coherent set of formula giving numerical expressions for precession quantities and mean elements of the Moon and the planets. First, using the notations of Lieske et al. (1977), we construct ...
A procedure of selection of meteoroids from major streams is suggested and applied to the IAU Lund photographic database modified by a check for internal consistency among orbital elements (3411 orbits). Limits for choice of stream members were defined by break points on the plots of the ...
The paper examines the orbital evolution of a group of 12 near-Earth asteroids with the mean motions being in resonance 3:1 with Jupiter, by the numerical integration over 100 000 years. The computation of six osculating elements has been done by forward integration taking into account the ...
A wide range of behavior is possible, from fast, low amplitude variations to systems in which eccentricities reach 0.9999 and inclinations 179.9 degrees. While the orbital elements evolve chaotically, at least one resonant argument always librates. We show that the HD 73526, HD 45364 and HD ...