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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.
In a two-body problem with inverse-square-law force, every orbit is a Kepler orbit. The eccentricity of this Kepler orbit is a non-negative number that defines its shape. The eccentricity may take the following values: Circular orbit: e = 0; Elliptic orbit: 0 < e < 1; Parabolic trajectory: e = 1; Hyperbolic trajectory: e > 1; The eccentricity e ...
This highly-eccentric three-week orbit takes it approximately 0.0523 AU of the star at periastron before swinging out to approximately 0.2665 AU at apastron. Its eccentricity is about the same as 16 Cygni Bb, a so-called "eccentric Jupiter". Until 2009, HD 17156 b was the transiting planet with the longest orbital period. [5]
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 ...
The companion of ASASSN-21js has an orbit of 13 000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass. [65] Smallest orbital separation SDSS J1730+5545 b: SDSS J1730+5545: 0.00139 AU [62] Most eccentric orbit: SGR 1935+2154 b: SGR 1935+2154: 0.992 or 0.994 [4] Highest orbital inclination: HD 204313 e: HD 204313: ...
The eccentricity of an orbit is a measure of how elliptical (elongated) it is. All the planets of the Solar System except for Mercury have near-circular orbits (e<0.1). [ 8 ] Most exoplanets with orbital periods of 20 days or less have near-circular orbits, i.e. very low eccentricity.
First calculation of WASP-14b's Rossiter–McLaughlin effect and so spin-orbit angle was −14 ± 17 degrees. [3] It is too eccentric for its age and so is possibly pulled into its orbit by another planet. [1] The study in 2012 has updated spin-orbit angle to 33.1 ± 7.4°. [4]
The orbit of an Earth-like planet would need to be centered within 0.68 AU [5] (around the orbital distance of Venus), which in a Keplerian system means a 240-day orbital period. In a 2006 simulation with the brown dwarf, 54 Piscium b's orbit "sweeps clean" most test particles within 0.5 AU, leaving only asteroids "in low-eccentricity orbits ...