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Eris has an orbital period of 559 years. [20] Its maximum possible distance from the Sun is 97.5 AU, and its closest is 38 AU. [20] As the time of perihelion is defined at the epoch chosen using an unperturbed two-body solution, the further the epoch is from the date of perihelion, the less accurate the result.
^ This object's rotation is synchronous with its orbital period, meaning that it only ever shows one face to its primary. ^ Objects' planetary discriminants based on their similar orbits to Eris. Sedna's population is currently too little-known for a planetary discriminant to be determined.
The orbital period (also revolution period) is the amount of time a given astronomical object takes to complete one orbit around ... 136199 Eris: 557 1.002 365.9 ...
Orbital period (years) Mean orbital speed (km/s) Inclination to ecliptic ... [90] [91] Triton is more massive than Eris or Pluto, has an equilibrium shape, ...
Combining Keck and Hubble observations, the orbit of Dysnomia was used to determine the mass of Eris through Kepler's third law of planetary motion. Dysnomia's average orbital distance from Eris is approximately 37,300 km (23,200 mi), with a calculated orbital period of 15.786 days, or approximately half a month. [2]
a dwarf planet, the third-largest-known trans-Neptunian object. Notable for its two known satellites, rings, and unusually short rotation period (3.9 h). It is the most massive known member of the Haumea collisional family. [28] [29] 136472 Makemake: a dwarf planet, a cubewano, and the fourth-largest known trans-Neptunian object [30] 136199 Eris
In astronomy, the rotation period or spin period [1] of a celestial object (e.g., star, planet, moon, asteroid) has two definitions. The first one corresponds to the sidereal rotation period (or sidereal day ), i.e., the time that the object takes to complete a full rotation around its axis relative to the background stars ( inertial space ).
In astrodynamics, the orbital eccentricity of an astronomical object is a dimensionless parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit , values between 0 and 1 form an elliptic orbit , 1 is a parabolic escape orbit (or capture orbit), and greater than ...