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Over hundreds of thousands of years, the eccentricity of the Earth's orbit varies from nearly 0.003 4 to almost 0.058 as a result of gravitational attractions among the planets. [3] Luna's value is 0.054 9, the most eccentric of the large moons in the Solar System.
TOI-2257 b is an extremely eccentric (0.496) [2] exoplanet in or near the circumstellar habitable zone of the star TOI-2257, 188 light-years away. It is likely a sub-Neptune exoplanet, with a mass of 5.71 Mearth and a radius of 2.19 Rearth. [3]
HD 80606 b has the most eccentric orbit of any known planet after HD 20782 b.Its eccentricity is 0.9336, comparable to Halley's Comet.The eccentricity may be a result of the Kozai mechanism, which would occur if the planet's orbit is significantly inclined to that of the binary stars.
HD 80606 b was considered the planet with the most eccentric orbit until the recent discovery. HD 80606 b has an eccentricity of 0.93 and a shorter orbit of 111 days, and it orbits in the same ...
With the exoplanet sample known in 2009, a group of astronomers estimated that "(1) around 35% of the published eccentric one-planet solutions are statistically indistinguishable from planetary systems in 2:1 orbital resonance, (2) another 40% cannot be statistically distinguished from a circular orbital solution" and "(3) planets with masses ...
16.4 +9.3 −4.0 M J [ 2 ] Iota Draconis b , formally named Hypatia (pronounced / h aɪ ˈ p eɪ ʃ i ə / or / h ɪ ˈ p eɪ ʃ ə / ), is an exoplanet orbiting the K-type giant star Iota Draconis about 101.2 light-years (31 parsecs , or nearly 2.932 × 10 14 km ) from Earth in the constellation Draco .
(40314) 1999 KR 16 is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 kilometers (158 miles) in diameter.It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESO ' s La Silla Observatory in northern Chile. [1]
However, the actual solution, assuming Newtonian physics, is an elliptical orbit (a Keplerian orbit). For these, it is easy to find the mean anomaly (and hence the time) for a given true anomaly (the angular position of the planet around the sun), by converting true anomaly f {\displaystyle f} to " eccentric anomaly ":