Aten asteroid
| Mars (M) Venus (V) Mercury (H) | Sun 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 2023, 2,445 Atens have been discovered, of which 256 are numbered, 13 are named, and 101 are classified as potentially hazardous asteroids.[2][3][4]
Description
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. Nearly all known Aten asteroids have an aphelion greater 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 semi-major axis of Mars (1.53 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]
NEO types
| Group | q | a | Q | ECA |
|---|---|---|---|---|
| Amors | > 1.017 | >1.0 | – | 
|
| Apollos | < 1.017 | >1.0 | – | 
|
| Atens | – | <1.0 | > 0.983 |
|
| Atiras | – | <1.0 | < 0.983 |
|
| For all NEOs q is < 1.3 AU; The orbit of Earth varies between 0.983 and 1.017 AU | ||||
See also
References
- ^ a b c "NEO Basics". NASA/JPL CNEOS. Retrieved 17 May 2018.
- ^ "Small-Body Database Query". Solar System Dynamics - Jet Propulsion Laboratory. NASA - California Institute of Technology. Retrieved 1 February 2023.
- ^ a b "List Of Aten Minor Planets (by perihelion distance)". Minor Planet Center. 17 May 2017. Retrieved 17 May 2017.
- ^ a b "Discovery Statistics – Cumulative Totals". NASA/JPL CNEOS. 16 May 2018. Retrieved 17 May 2018.
- ^ "99942 Apophis (2004 MN4) Earth Impact Risk Summary". NASA. Archived from the original on 11 May 2013.
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