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The Aten group compared to the orbits of the terrestrial planets of the Solar System.      Mars (M)   Venus (V)   Mercury (H)     Sun   Aten asteroids   Earth (E)
The Aten group compared to the orbits of the terrestrial planets of the Solar System.
  Mars (M)
  Venus (V)
  Mercury (H)
  Aten asteroids
  Earth (E)

The Aten asteroids are a dynamical group of asteroids whose orbits bring them into proximity with Earth. By definition, Atens are Earth-crossing asteroids (a < 1.0 AU and Q > 0.983 AU).[1] The group is named after 2062 Aten, the first of its kind, discovered on 7 January 1976 by American astronomer Eleanor Helin at Palomar Observatory. As of 2019, 1490 Atens have been discovered, of which 12 are named.[2] Many Atens are classified as potentially hazardous asteroids.[3][4]

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Aten asteroids are defined by having a semi-major axis (a) of less than 1.0 astronomical unit (AU), the roughly average distance from the Earth to the Sun. They also have an aphelion (Q; furthest distance from the Sun) greater than 0.983 AU.[1] This defines them as Earth-crossing asteroids as the orbit of Earth varies between 0.983 and 1.017 AU.

Asteroids' orbits can be highly eccentric. An Aten orbit need not be entirely contained within Earth's orbit, and nearly all known Aten asteroids have an aphelion greater than 1 AU although their semi-major axis is less than 1 AU. Observation of objects inferior to the Earth's orbit is difficult, and this difficulty may contribute to sampling bias in the apparent preponderance of eccentric Atens. Aten asteroids account for only about 7.4% of the known near-Earth asteroid population.[4] Many more Apollo-class asteroids are known than Aten-class asteroids, possibly because of the sampling bias.

The shortest semi-major axis for any known Aten asteroid is 0.580 AU, for object 2016 XK24.[3] The Aten asteroid with the smallest known perihelion is also the one with the highest known eccentricity: (137924) 2000 BD19 has an orbit with an eccentricity of 0.895, which takes it from a perihelion of 0.092 AU, well within Mercury's orbit, to an aphelion of 1.66 AU, which is greater than the perihelion of Mars (1.38 AU). For a brief time near the end of 2004, the asteroid 99942 Apophis (then known only by its provisional designation 2004 MN4) apparently posed a threat of impacting Earth in 2029 or 2036, but earlier observations were found that eliminated those possibilities.[5]


As of 2019 there are 18 known Atira asteroids (also known as Apoheles asteroids),[4][6] traditionally listed as a subgroup of Atens,[3] but often regarded as a separate asteroid class.[1] Unlike Atens (Q > 0.983 AU), Atiras permanently reside within, and do not cross, Earth's orbit.(Q < 0.983 AU).[1]

Definition of NEO subgroups in AU[1]
Group q a = 1 Q ECA
Amors > 1.017 larger Red XN
Apollos < 1.017 larger Green tickY
Atens smaller > 0.983 Green tickY
Atiras smaller < 0.983 Red XN
For all NEOs q is < 1.3 AU; The orbit of Earth varies between 0.983 and 1.017 AU

See also


  1. ^ a b c d e "NEO Basics". NASA/JPL CNEOS. Retrieved 17 May 2018.
  2. ^ "JPL Small-Body Database Search Engine". NASA/JPL. Retrieved 19 Jan 2019.
  3. ^ a b c "List Of Aten Minor Planets (by perihelion distance)". Minor Planet Center. 17 May 2017. Retrieved 17 May 2017.
  4. ^ a b c "Discovery Statistics – Cumulative Totals". NASA/JPL CNEOS. 16 May 2018. Retrieved 17 May 2018.
  5. ^ "99942 Apophis (2004 MN4) Earth Impact Risk Summary". NASA. Archived from the original on 2013-05-11.
  6. ^ "JPL Small-Body Database Search Engine: Q < 0.983 (AU)". JPL Solar System Dynamics. Retrieved 17 May 2018.

This page was last edited on 3 April 2019, at 20:29
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