Planets that form in circumstellar disks are expected to have nearly circular orbits, although gravitational interactions in a system of two or more planets could generate high-eccentricity orbits. Here we suggest that the eccentric orbit of 16 Cyg Bb arises from gravitational interactions with the ...
A perfectly circular orbit has an eccentricity of zero. Elliptical orbits have values between 0 and 1 with higher values indicating a more eccentric orbit. An eccentricity of exactly 1 is a parabolic orbit and anything greater than that is a hyperbolic orbit. The orbits of the planets are ...
- 《Journal of Geophysical Research Planets》 被引量: 79发表: 2010年 Deorbiting Performance of Bare Electrodynamic Tethers in Inclined Orbits BARE electrodynamic tethers (EDTs) provide a relatively simple and effective tool for rapidly deorbiting spent satellites and rocket stages in low Earth or.....
If the migration rate is fast, the resonant pair can evolve into a family of 2:1 eccentricity resonances different from those found by Lee. This new family has outer orbital eccentricity e 2 0.4-0.5, asymmetric librations of both eccentricity resonance variables, and orbits that intersect if ...
Astronomical forcing of Earth’s climate is embedded in the rhythms of stratigraphic records, most famously as short-period (104–105 year) Milankovitch cycles. Astronomical grand cycles with periods of millions of years also modulate climate variability
Data collected on the orbital eccentricities of extrasolar planets has surprised most researchers: 90% have an orbital eccentricity greater than that found within the Solar System, and the average is fully 0.25. Datele colectate pe excentricități de planete extrasolare-a surprins pe cei ...
area of an ellipse Orbits of Planets as ellipses Translate ellipse images Worksheet Version of this Web page (same questions on a worksheet) The eccentricity of an ellipse is a measure of how nearly circular the ellipse. Eccentricity is found by the following formula eccentricity = c/a where ...
Transiting exoplanets in multi-planet systems have non-Keplerian orbits which can cause the times and durations of transits to vary. The theory and observations of transit timing variations (TTV) and transit duration variations (TDV) are... E Agol,F Dan - Handbook of Exoplanets, Edited by Ha...
The behavior of the system depends solely on the mass ratio μ of the binary components and the initial distance ratio of the planet relative to the stellar separation distance noting that the stellar components move on circular orbits. Our study indicates that orbital instability occurs when the ...
parable time scales). Around Ups And and HD168443, the planets’ orbits are not in mean motion resonances so that their semi-major axes are conserved while their eccentricity and longitude of periapse modulate over some characteristic secular time scale (Murray & Der- ...